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PHILOSOPHICAL  SOCIETY  OF   WASHINGTO^U- 

V^  BULLETIN  VOL.  XI,  pp.  275-358. 


THE  PROGRESS 


OF 


METEORIC  ASTRONOMY 


IN 


AMERI 


BY 


JOHN  ROBIE  EASTMAN 


HEAD  BEFORE  THK  PHILOSOPHICAL  SOCIETY  OF   WASHINGTON. 
APRIL  12,  1800. 


WASHINGTON  : 

PUBLISHED  BY  THE  SOCIETY 
JULY,  1890. 


#8741 


THE   PROGRESS   OF   METEORIC   ASTRONOMY   IN 

AMERICA. 


BY 


JOHN  ROBIE  EASTMAN. 


[Read  before  tho  Society  April  12,  1890.] 


TABLE  OF  CONTENTS. 

Page. 

Introduction 270 

Abstracts  of  Theories 278 

Authors : 

Rev.  Thomas  Clap 278 

Dr.  W.  G.  Reynolds 278 

Prof.  Edward  Hitchcock 279 

Prof.  D.  Olmstead 279 

E.  C.  Herrick 281 

Prof.  Benjamin  Peirce 281 

Prof.  S.  C.  Walker 281 

Prof.  Peter  A.  Browne 282 

Prof.  J.  Lawrence  Smith 283 

Dr.  B.  A.  Gould 283 

Prof.  H.  A.  Newton 285 

Prof.  A.  C.  Twining 285 

Prof,  II.  A.  Newton 285 

Prof.  A.  C.  Twining 28G 

B.  V.  Marsh 28G 

Prof.  II.  A.  Newton « 287 

Prof.  Daniel  Kirkwood 290 

Prof.  H.  A.  Newton 290 

Prof.  S.  Newcomb 291 

Prof.  W.  Harkness__ 291 

Prof.  Daniel  Kirkwood 291 

Jacob  Ennis 291 

Prof.  Pliny  Earle  Chase 292 

Prof.  H.  A.  Newton 292 

Prof.  J.  W.  Mallet 292 

34— Bull.  Phil.  Hoc.,  Wash.,  Vol.  11.  (275) 


276  EASTMAN. 

Page. 
Authors : 

Prof.  A.  W.  Wright 292 

Prof.  H.  A.  Newton 292 

Prof.  H.  A.  Newton 297 

Examination  of  Theories 298 

Meteors 298 

Comets 300 

Comets  and  Meteors •_ 302 

Loclcyer's  Theories 305 

Huggins  on  the  Spectra  of  the  Aurora  and  of  Nebulas 310 

Liveing  and  Dewar  on  the  Spectra  of  Nebulae  and  of  Magnesium,  310 

Conclusions 311 

Observations  of  Meteors 312 

Catalogues :;i:; 

I.  Observed  Meteorites 3HJ 

II.  Discovered  Meteorites,  date  of  discovery  given 318 

III.  Discovery  of  Meteorites,  date  of  discovery  unknown 322 

IV.  Meteor  Showers :52» 

V.  Sporadic  Meteors 33G 


INTRODUCTION. 

The  progress  of  Meteoric  Astronomy  through  its  succes- 
sive stages  of  development  has  been  so  peculiar  in  America, 
especially  in  the  United  States,  that,  unlike  almost  all  4 he 
other  branches  of  Astronomy  and  Physics,  its  advance  may 
be  thoroughly  discussed  with  very  little  reference  to  the  im- 
portant growth  which  it  has  made  in  Europe. 

From  the  nature  of  the  phenomena  it  is  evident  that  the 
apparition  and  fall  of  meteors  must  have  compelled  the  at- 
tention of  mankind  through  all  ages,  but  the  earliest  records 
are  at  least  obscure.  While  there  may  be  some  claim  to 
authenticity  in  the  early  allusions  to  what  was  apparently 
meteoric  phenomena,  there  seem  to  be  no  trustworthy  obser- 
vations until  about  600  B.  C. 

From  that  time  the  falls  of  a  great  number  of  meteors  and 
meteorites  were  recorded  with  more  or  less  accuracy  and 
detail,  but  no  special  attention  was  attracted  to  the  observa- 
tion and  study  of  such  phenomena  until  the  publication  of 
a  paper  in  1794,  by  Chladni,  on  a  mass  of  meteoric  iron 


PROGRESS   OF   METEORIC  ASTRONOMY    IN  AMERICA.       277 

found  in  Siberia  by  Dr.  Pallas,  a  well-known  naturalist. 
About  this  time  several  noted  meteorites  fell  in  Europe,  and 
in  1802  Edward  Howard  published  in  the  Philosophical 
Transactions  a  paper  entitled  "  Experiments  and  observa- 
tions on  certain  stony  substances  which  at  different  times 
are  said  to  have  fallen  on  the  earth."  This  paper  contains, 
probably,  the  account  of  the  first  chemical  analysis  of  a 
meteorite  ever  made. 

Nearly  all  the  publications  referring  to  meteors,  both  in 
Europe  and  America,  up  to  the  year  1833  were  confined  to 
vague  theories  and  brief  speculations  with  regard  to  their 
origin. 

The  very  important  meteoric  shower  on  the  morning  of 
April  20,  1803,  was  the  first  well-defined  phenomenon  of  that 
class  in  this  country  of  which  there  seems  to.be  any  record. 
There  is  no  evidence  that  it  was  well  observed  except  at 
Portsmouth,  N.  H.,  and  at  Richmond,  Va.,  and  no  recurrence 
of  this  shower  of  any  notable  magnitude  has  since  been  ob- 
served. Graphic  accounts  of  this  phenomenon  were  printed 
in  "  The  New  Hampshire  Gazette,"  of  Portsmouth,  N.  H., 
May  31,  1803,  and  in  "  The  Virginia  Gazette  and  General 
Advertiser,"  of  Richmond,  Va.,  May  23,  1803,  but  appar- 
ently no  scientific  interest  or  discussion  was  developed. 

The  wonderful  display  of  meteors  on  the  morning  of  No- 
vember 14,  1833,  which  was  seen  throughout  the  Atlantic 
coast  of  the  United  States,  gave  a  decided  impulse  to  the 
study  of  the  subject  and  suddenly  brought  the  principal 
American  observers  into  prominence. 

The  serious  study  of  meteoric  phenomena  in  America 
may  be  said  to  date  from  this  epoch. 

The  earliest  studies  immediately  developed  theories,  more 
or  less  fantastic,  to  account  for  the  varied  but  startling  dis- 
play in  the  heavens. 

The  first  theories,  derived  from  only  a  few  facts,  naturally 
presented  the  greatest  range  of  speculation. 

As  phenomena  multiplied,  the  limits  of  speculation  were 


278  EASTMAN. 

notably  contracted,  and  in  1834  the  germ  of  the  true  theory 
of  meteoric  motion  was  presented,  but  not  developed. 

The  most  accurate  idea  of  the  progress  of  the  science  of 
Meteoric  Astronomy  can  be  obtained,  without  doubt,  from 
an  examination  of  the  principal  theories. 

ABSTRACTS  OF  THEORIES. 

The  following  abstracts  of  these  theories  are  presented  in 
chronological  order,  and  in  each  case  the  language  of  the 
author  is  employed  if  practicable. 

Probably  the  first  paper  printed  in  this  country  which  ad- 
vances any  theory  of  the  nature  or  the  motion  of  meteors 
was  written  by  Eev.  Thomas  Clap,  ex-president  of  Yale  Col- 
lege, and  was  printed  in  Norwich,  Connecticut,  in  1781.  He 
concluded  that  "  our  observations  have  heretofore  been  so 
imperfect  as  that  we  cannot  easily  determine  minute  circum- 
stances; but  the  general  theory  seems  highly  probable,  if 
not  certain,  that  these  superior  meteors  are  solid  bodies,  half 
a  mile  in  diameter,  revolving  around  the  earth  in  long 
ellipses,  their  least  distance  being  about  twenty  or  thirty 
miles;  that  by  their  friction  upon  the  atmosphere  they 
make  a  constant  rumbling  noise  and  collect  electrical  lire, 
and  when  they  come  nearest  the  earth  or  a  little  after,  being 
then  overcharged,  they  make  an  explosion  as  loud  as  a 
large  cannon." 

In  1819  W.  G.  Reynolds,  M.  7).,  of  Middletown  Point,  N. 
J.,  published  a  paper  *  advocating  the  theory  that  "  Meteors 
proceed  from  the  earth.  They  arise  from  certain  combina- 
tions of  its  elements  with  solar  heat,  and  meteoric  stones  are 
the  necessary  results  of  the  decomposition  of  these  combina- 
tions." 

After  the  shower  of  1833  elaborate  accounts  of  the  event 
were  written  by  several  scientific  observers,  and  various  con- 
clusions and  theories  were  deduced. 

Prof.  Edward  Hitchcock?  of  Amherst  College,  Mass.,  con- 
1  A.  J.  S.,  Ip  266.  2  A.  J.  S.,  XX  Vp  354. 


PROGRESS  OF   METEORIC  ASTRONOMY    IN  AMERICA.       279 

eluded  that  "  there  was  a  point  from  which  most  of  the 
meteors  seemed  to  emanate  ;  that  this  radiant  corresponded 
to  that  point  in  the  dome  of  the  heavens  to  which  the  mag- 
netic needle  would  point  if  left  free  to  move  vertically  and 
horizontally,  and  that  meteors  are  only  modifications  of  the 
Aurora  Borealis." 

Prof.  D.  Olmstead,1  of  Yale  College,  discussed  at  length  the 
meteors  of  November  13,  1833,  with  the  following  conclu- 
sions : 

"  1st.  The  meteors  originated  beyond  the  limits  of  our  at- 
mosphere and  fell  towards  the  earth,  in  straight  and  nearly 
parallel  lines,  from  a  point  2,238  miles  above  the  surface  of 
the  earth. 

"  2d.  Their  velocity  on  entering  the  earth's  atmosphere  was 
about  four  miles  per  second: 

"  3d.  They  consisted  of  light,  transparent,  combustible  mat- 
ter, and  took  fire  and  were  consumed  in  traversing  the  at- 
mosphere." 

Prof.  Olmstead  finally  concluded  that  "  the  meteors  of 
November  13  consisted  of  portions  of  the  extreme  parts  of  a 
nebulous  body  which  revolves  around  the  sun  in  an  orbit 
interior  to  that  of  the  earth,  but  little  inclined  to  the  plane 
of  the  ecliptic,  having  its  aphelion  near  to  the  earth's  path 
and  having  a  periodic  time  of  182  days,  nearly." 

After  discussing  the  November  meteors  of  1836,  Prof. 
Olmstead2  concluded  that  "  the  zodiacal  light  might  be  the 
source  of  those  meteors,  and  therefore  was  not  a  portion  of 
the  sun's  atmosphere,  but  a  nebulous  or  cometary  body  re- 
volving around  the  sun  within  the  earth's  orbit  nearly  in 
the  plane  of  the  solar  equator,  approaching  at  times  very 
near  to  the  earth,  and  having  a  periodic  time  of  either  one 
year  or  half  a  year,  nearly." 

On  the  28th  of  April,  1840,  Mr.  E.  C.  HerricP  read  before 
the  Connecticut  Academy  of  Arts  and  Sciences  a  paper  on 

1  A.  J.  S.,  XXVI^  132.  2  At  j.  Si>  XXXIX,  386. 

3  A.  J.  S.,  XLt,  349. 


280 


EASTMAN. 


"The  history  of  star-showers  of  former  times,"  in  wliu-h  he 
presented  a  brief  account  of  all  the  records  he  had  been  al»lv 
to  find,  together  with  the  following  tabular  chronological 
account  of  star-showers,  where  the  dates  arc  reduced  to 
gorian  style : 

Chronological  List  of  Star-Showers. 


Number. 

Date. 

Number. 

Date. 

1 

B.  C.  1768. 

21 

A.  D.  1060. 

2 

B.  C.     686. 

22 

"       1090. 

3 

A.  D.        7. 

23 

"       1094. 

,  4 

"       532. 

24 

"       1095,  April  10. 

5 

"       558. 

25 

"       1096,  April  10  (?). 

6 

"       585,  September  6  (?). 

26 

11       1106,  February  19. 

7 

"       Gil. 

27 

"       1122,  April  11. 

8 

"       744  or  747. 

28 

"       1199,  October  (?). 

9 

"       750. 

29 

"       1202,  October  L'li. 

10 

764  (?),  March. 

30 

"       1243,  Augu.st  *J. 

11 

"        705,  January  8. 

31 

"       1366,  October  30. 

12 

"       829. 

32 

"       1398. 

13 

"       855,  October  21. 

33 

"       1399,  October  (?). 

14 

"       899,  November  18. 

34 

"       1635  or  1636. 

15 

"       901,  November  30. 

35 

"       1743,  October  15. 

16 

"       902,  October  30. 

36 

"       1799,  November  12. 

17 

"       912  or  913. 

37 

"       1803,  April  20. 

18 

"       931  or  934,  October  19. 

38 

"       1832,  November  13. 

19 

"       935,  October  (?). 

39 

"       1833,  November  13. 

20 

"     1029,  July  or  August. 

PROGRESS  OF   METEORIC  ASTRONOMY   IN  AMERICA.      281 

Of  the  theory  of  meteors,  Mr.  Herrick  wrote : 

"  The  most  probable  hypothesis  is  that  there  are  revolving 
around  the  sun  millions  of  small  planetary  and  nebulous 
bodies  of  various  magnitudes  and  densities,  and  that  when 
any  of  these  dart  through  our  atmosphere  they  become 
ignited  and  are  seen  as  shooting-stars." 

In  discussing  a  paper  on  meteors  by  Prof.  Erman  (Schu- 
macher's Ast.  Nach.  No.  385)  Pro/.  Benjamin  Peirce?  after 
pointing  out  an  error  in  Erman's  work,  concludes  in  these 
words  :  "  The  plane  of  the  meteors  cannot  differ  much  from 
that  of  the  ecliptic,  and  their  relative  velocity  cannot  exceed 
one-third  of  the  earth's  velocity.  A  ring  so  nearly  in  the 
plane  of  the  earth's  orbit  must  be  subject  to  great  perturba- 
tions ;  and,^f  there  is  one,  I  think  that  no  observations  which 
we  can  make  will  enable  us  to  calculate  its  motions  with  any 
degree  of  accuracy." 

On  January  15,  1841,  Prof.  S.  C.  Walker*  read  a  paper 
before  the  American  Philosophical  Society,  "  On  the  peri- 
odical meteors  of  August  and  November,"  in  which  the  fol- 
lowing points  were  discussed  : 

The  relative  velocities  of  meteors ; 

The  relative  directions  of  meteors  in  space ; 

The  periodical  or  anniversary  display  of  meteors  ; 

The  respective  plausibilities  of  the  hypotheses  of  a  single 
cluster  with  a  half-yearly  or  yearly  period,  or  that  of  a  con- 
tinuous ring  for  the  periodical  meteors  of  August  and  No- 
vember ; 

The  theories  of  aerolites  and  shooting-stars ; 

The  variation  of  the  relative  velocity  and  of  the  conver- 
gent point ; 

And  principally  the  investigation  of  formula  for  com- 
puting the  elliptic  elements  of  the  orbit  of  a  meteor  from  its 
observed  relative  velocity  and  direction. 

In  1844  an  "  Essay  on  Solid  Meteors  and  Meteoric  Stones  " 

1  Trans.  Am.  Phil.  Soc.,  VIII2,  83. 

2  Trans.  Am.  Phil.  Soc.,  VIII2)  87. 


282  EASTMAN. 

was  published  by  Prof.  Peter  A.  Browne,  of  La   Fayette 
College. 

The  author  devoted  the  first  and  larger  portion  of  his 
paper  to  proving  the  solidity  of  meteors. 

The  latter  portion  of  his  essay  was  confined  to  the  exami- 
nation and  rejection  of  all  the  theories  previously  advanced, 
which,  briefly  stated,  were  : 

'  1st.  t)r.  Halley's  theory  that  meteors  were  nothing  but  a 
stratum  of  inflammable  vapor,  gradually  raised  from  the 
earth  and  accumulated  in  an  elevated  region,  which  sud- 
denly took  fire  at  one  end  and  the  progress  of  the  flame 
along  the  stratum  produced  the  apparent  motion  of  the 
meteor. 

2d.  The  theory  in  Luke  Howard's  Meteorology  that  hy- 
drogen gas  dissolves  various  bodies,  even  iron,  and  that  is 
evolved,  mixed  with  carbon  in  the  gaseous  state,  from  the 
earth  in  large  quantities,  is  collected  in  vast  fields  in  the  air, 
is  fired  by  electric  explosions,  and,  the  gasses  burning  out, 
they  let  fall  the  earthy  and  metallic  contents  precipitated 
and  agglutinated  as  we  find  them  in  aerolites. 

3d.  Prof.  Soldani's  theory  that  meteoric  stones  are  gener- 
ated in  the  air  by  a  combination  of  mineral  substances  which 
had  risen  as  exhalations  from  the  earth. 

4th.  Dr.  Reynolds'  theory,  previously  given  in  this  paper. 

5th.  Dr.  Blagden's  theory  that  meteors  are  electrical  phe- 
nomena. 

6th.  The  theory  of  Patrick  Murray  that  meteors  originate 
in  the  local  atmosphere  of  the  earth,  and  their  explosions  are 
due  to  electrical  action. 

7th.  The  theories  of  Brewster  and  La  Grange  that  meteors 
are  bodies  thrown  off  from  the  earth  by  volcanic  action. 

8th.  The  theories  of  Hutton  and  La  Place  that  meteors 
are  thrown  from  volcanoes  in  the  moon. 

9th.  Newton's  -theory  that  they  proceed  from  the  tail  of  a 
comet. 

10th.  They  are  terrestrial  comets — a  theory  maintained  by 
Professors  Clap  and  Day  and  by  Carvallo. 


PROGRESS  OF   METEORIC  ASTRONOMY   IN  AMERICA.      283 

llth.  The  theory  that  they  were  solids  that  have  been 
floating  in  space  from  the  beginning ;  advocated  by  Chladni, 
Franklin,  and  Bittenhouse. 

12th.  The  theory  of  Olbers  that  they  are  fragments  of  an 
exploded  planet. 

13th.  The  theory  of  Quetelet  that  they  belong  to  a  zone 
through  which  the  earth  passes  annually. 

14th.  The  theory  of  Boubee  that  they  are  fragments  of  an 
exploded  comet. 

These  theories  are  all  rejected  as  disproved  or  absurd ;  but 
the  author  advances  no  theory  as  a  substitute.  He  announces, 
however,  that,  to  his  mind,  "  the  most  probable  supposition 
yet  made  is  that  the  solid  meteors  may  possibly  emanate 
from  the  sun,"  though  no  serious  attempt  is  made  to  prove 
the  proposition. 

In  a  paper  read  by  Pro/.  J.  Lawrence  Smith  before  the 
American  Association  for  the  Advancement  of  Science,  in 
April,  1854,  the  author l  advocated  the  theory  of  the  lunar 
origin  of  meteors,  which  he  stated  as  follows :  "  The  moon 
is  the  only  large  body  in  space,  of  which  we  have  any  knowl- 
edge, possessing  the  requisite  conditions  demanded  by  the 
physical  and  chemical  properties  of  meteorites ;  and  they 
have  been  thrown  off  from  that  body  by  volcanic  action 
(doubtless  long  since  extinct),  and,  encountering  no  gaseous 
medium  of  resistance,  reached  such  a  distance  as  that'  the 
moon  exercised  no  longer  a  preponderating  attraction,  the  de- 
tached fragment  possessing  an  orbital  motion  and  an  orbital 
velocity  which  it  had  in  common  with  all  parts  of  the  moon, 
but  now  more  or  less  modified  by  the  projectile  force  and  new 
condition  of  attraction  in  which  it  was  placed  in  reference 
to  the  earth,  acquired  an  independent  orbit  more  or  less 
elliptical.  This  orbit,  necessarily  subject  to  great  disturbing 
influences,  may  sooner  or  later  cross  our  atmosphere  and  be 
intercepted  by  the  body  of  the  globe." 

In  1859  2  Dr.  B.  A.  Gould  read  a  paper  before  the  Ameri- 

1  A.  J.  S.,  XIX2,  343.  2  Proc.  A.  A.  A.  S.  1859,  181. 

35— Bull.  Phil.  Soc.  Wash.,  Vol.  11. 


284  EASTMAN. 

can  Association  for  the  Advancement  of  Science  to  disprove 
the  theory  that  meteors  had  their  origin  in  lunar  valcanoes. 

Assuming  that  a  lunar  volcano  may  eject  masses  of  matter 
with  the  requisite  velocity  to  pass  beyond  the  region  where 
the  lunar  gravitation  predominates  over  the  terrestrial  and 
the  masses  become  obedient  to  the  earth's  attraction,  Dr. 
Gould  examines  in  detail  the  consequences  to  which  the 
theory  of  the  lunar  origin  of  meteorites  would  necessarily 
lead,  and  presents  his  conclusions  as  follows : 

"  From  the  foregoing  considerations  we  are  warranted  in 
assuming  that  for  every  body  expelled  from  lunar  volcanoes 
with  a  force  adapted  for  throwing  to  the  earth  an  aerolite  of 
average  dimensions  there  are,  in  probability,  at  the  very 
least  one  hundred  and  eighty  bodies  expelled  with  foiv.-s 
not  thus  adapted;  that  for  every  mass  ejected  with  the  av- 
erage force  of  a  lunar  volcano  and  striking  the  earth,  there 
are  at  least  one  hundred  and  eighty  masses  of  inadequate 
dimensions  ejected ;  and  that  for  any  given  combination  of 
volcanic  force  and  projected  mass,  the  region  of  the  lunar 
surface,  whence  the  mass  may  reach  the  earth,  is  exceeded 
in  extent  by  the  tract  of  the  lunar  surface  whence  this  would 
be  impossible,  in  the  ratio  of  fifty  to  one.  Combining  these 
several  individual  probabilities,  it  will  readily  be  perceived 
that  not  more  than 

3*0    X  y|-jy  X  T^-  =  T6T¥Oinr 

of  all  the  ejected  lava  masses,  or  about  3  in  5,000,000  of  ouch 
possible  size,  would  probably  ever  reach  the  earth  as  aero- 
lites; nor  is  this  an  unsafe  estimate.  It  is  a  very  guarded 
one,  and  the  fraction  ^ooTifFo  would  be  more  likely  to  be 
correct.  Now,  can  we  regard  it  as  probable  that  the  moon 
has  parted  with  so  large  an  amount  of  matter  as  nearly,  if 
not  quite,  two  million  times  the  combined  mass  of  all  the 
aerolites  which  have  fallen  to  the  earth?  I  think  not. 
Even  of  those  known  to  have  fallen  there  are  more  than  five 
hundred  of  various  weights,  one  of  them  having  a  mass  of 
thirty  thousand  pounds.  The  tokens  of  such  a  mass  of 
gravitative  matter  as  this  would  imply  could  not  fail  to  be 


PROGRESS   OF   METEORIC  ASTRONOMY    IN  AMERICA.      285 

legibly  inscribed  in  the  unerring  and  enduring  records  of 
our  system.  They  would  preclude  the  accordance  which 
is  found  to  exist  between  the  present  lunar  theory  and  the 
ancient  observations.  They  would  be  found  to  be  incon- 
sistent with  the  known  values  of  precession  and  nutation. 
They  might,  indeed,  almost  be  said  to  be  incompatible  with 
the  present  mass  of  the  moon." 

From  the  observations  of  the  meteor  of  November  15, 1859, 
Prof.  H.  A.  Newton1,  of  Yale  College,  concluded  that  it  must 
have  moved  in  a  hyperbolic  orbit,  and  that  we  have,  there- 
fore, two  sources  of  meteors — the  solar  system  and  stellar 
space. 

With  regard  to  the  periodic  meteors  of  August,  Mr.  A.  C. 
Twining*,  of  New  Haven,  concluded  that  "  the  radiant  is 
probably  capable  of  a  far  more  exact  determination  than  is 
ordinarily  supposed  or  than  could  have  been  anticipated, 
and  it  is  apparently  subject  to  a  motion  of  several  degrees 
from  day  to  day,  and  a  motion  which  exhibits  some  remark- 
able points  of  agreement  in  the  comparison  of  one  year's 
positions  with  those  of  other  years." 

From  a  discussion  of  the  peculiar  characteristics  of  the 
August  meteors  Prof.  H.  A.  Newton3  came  to  the  following 
conclusions : 

1st.  The  individual  meteors  are  cosmical  bodies. 

2d.  They  are  permanent  members  of  the  solar  system,  re- 
volving about  the  sun  in  elliptic  orbits. 

3d.  The  direction  and  velocity  of  the  relative  motion,  and 
therefore  of  the  absolute  motion  of  the  individual  bodies,  are 
nearly  the  same. 

4th.  The  whole  group  forms  what  may  be  considered  a 
ring  or  disk  around  the  sun. 

5th.  The  periodic  time  is  two  hundred  and  eighty-one 
days. 

1  A.  J.  S.,  XXX2,  186.  2  A.  j.  St>  XXXII2>  444. 

3  A.  J.  S.,  XXXII2,  448. 


286  EASTMAN. 

In  the  same  paper  Professor  Newton  estimates  the  whole 
number  of  meteors  in  the  August  ring  as  300,000,000,000,000. 

In  March,  1862,  A.  C.  Twining1,  published  a  paper  entitled 
"  Investigations  respecting  the  phenomena  of  meteoric  rings 
as  affected  by  the  earth,"  and  arrived  at  the  following  con- 
clusions :  "  The  position  of  the  node  of  the  ring  cannot  be 
shifted  by  the  earth's  action  more  than  a  degree  or  two  in 
half  a  million  of  years ;  there  is  an  appreciable  change  of 
radiant  positions,  relative  to  locality  on  the  earth's  surface 
and  to  the  hour  of  the  day,  whose  maximum  is  about  3  J°  be- 
tween the  extremes  and  to  which  the  extremes  approach  ;  the 
terrestrial  disturbance  is  sufficient  to  affect  the  perihelion 
distance  of  the  meteors  by  many  millions  of  miles  and  to 
expand  the  ring  to  a  corresponding  breadth  at  the  ascend- 
ing node ;  also  to  collect  together  in  orbits,  of  similar  ele- 
ments, those  meteors  which  are  similarly  affected  in  respect 
of  radiant  positions ;  and  terrestrial  disturbances  do  not  ap- 
pear sufficient  to  draw  off  meteors  into  permanently  erratic 
orbits;  so  that,  unless  in  exceptional  instances,  meteors  an- 
not  lost  to1  the  ring  other  than  those  which  the  atmosphere 
absorbs  or  arrests.  If  meteors  are  partially  arrested  without 
being  dissipated  in  an  excessively  tenuous  upper  medium 
it  may  be  possible  that  the  ordinary  and  unconformablc 
meteors  are  such  as  have  missed  a  return  to  the  ring  under 
the  effect  of  atmospheric  retardation." 

Mr.  Twining  appends  the  suggestion  that,  "  perhaps  comets 
whose  vastly  extended  atmospheres  or  heads  around  the 
nucleus,  although  greatly  attenuated  are  perhaps  competent 
to  arrest  meteors  completely,  may  be  found  in  rare  instances 
to  have  been  disturbed  by  impact  with  a  meteoric  ring  whose 
mere  attractive  influence  it  would  not  be  possible  to  detect." 

In  1863,  Mr.  B.  V.  Marsh?  of  Philadelphia,  published  a 
pq,per  on  "  The  luminosity  of  meteors  as  affected  by  latent 
heat,"  in  which  he  arrived  at  the  following  results:  "The 
upper  regions  of  the  atmosphere,  even  to  its  utmost  limit, 

1  A.  J.  S.,  XXXIII2,  244.  2  A>  j.  s<>  XXXVI2,  92. 


PROGRESS   OF    METEORIC  ASTRONOMY    IN  AMERICA.      287 

are  grand  reservoirs  of  latent  heat  most  admirably  adapted 
to  the  protection  of  the  earth  from  collision  with  bodies  ap- 
proaching it  with  planetary  velocity  from  without.  The 
intruder  is  instantly  surrounded  with  a  fiery  envelope  heated 
to  the  greatest  conceivable  intensity ;  its  surface  is  burned  off 
or  dissipated|into  vapor;  the  sudden  expansion  of  the  stratum 
immediately  beneath  the  burning  surface  tears  the  body  into 
fragments,  each  of  which,  retaining  its  planetary  velocity,  is 
instantly  surrounded  by  a  similar  envelope,  which  produces 
like  effects,  and  so  on  until,  in  most  cases,  the  whole  is  burned 
up  or  vaporized."  A  second  paper  on  the  same  subject,  and 
of  similar  import,  was  published  by  Mr.  Marsh  in  the  Pro- 
ceedings of  the  American  Philosophical  Society,  vol.  XIV, 
114. 

From  an  examination  of  the  list  of  November  meteor 
showers  from  A.  D.  902  to  A.  D.  1833  Pro/.  //.  A.  Newton1 
concluded  that  "the  star-shower  has  a  motion  along  the 
sidereal  year  of  one  day  in  seventy  years,  and  also  that  the 
shower  has  a  period  of  about  a  third  of  a  century.  This 
precession  seems  to  imply  that  the  orbit  of  the  body  furnish- 
ing these  meteors  has  only  a  small  inclination  to  the  ecliptic, 
and  that  the  motion  is  retrograde.  The  small  distance  of 
the  radiant  from  the  point  to  which  the  earth  is  moving, 
viz.,  7°,  confirms  this  conclusion." 

In  an  article  on  the  peculiarities  of  the  November  meteors, 
Prof.  H.  A.  Newton^  arrived  at  the  following  conclusions : 
"  The  length  of  the  annual  period  as  determined  from  the 
showers  in  A.  D.  902  and  1833,  reckoning  233  leap  years, 
19  odd  days,  and  adding  six  hours  for  difference  of  longi- 
tude, is  365  +  C*33^;9'2*) ,  or  365.271  days.  The  length  of  the 
cycle  is  33.25  years. 

"  The  length. of  the  part  of  a  cycle  during  which  showers 
may  be  expected  may  be  five  or  six  years  or,  for  extraordi- 
nary displays,  at  least  2.25  years.  The  supposition  of  a 
ring  of  uniform  density  throughout  its  circuit  seems  im- 
probable. 

1  A.  J.  S.,  XXXVI2,  300.  3  A.  J.  S.,  XXXVIIIa,  53. 


288  EASTMAN. 

"  The  elements  of  the  mean  of  the  orbits  of  the  different 
groups  composing  the  partial  ring  are : 

Semi-major  axis  =  0.98049, 
Inclination          =  17°, 
and  the  ring  is  nearly  circular. 

"  The  velocity  with  which  these  bodies  enter  the  earth's 
atmosphere  is  about  20.17  English  miles  per  second." 

The  most  elaborate  American  paper  on  meteors  up  to  the 
date  of  its  publication  was  prepared  in  1865  by  Prof.  77.  A. 
Newton,1  who  discussed  the  subject  under  the  following  divi- 
sions, the  conclusions  being  briefly  stated  in  each  case : 

"  1st.  The  average  altitude  of  the  middle  points  of  the 
luminous  portions  of  the  meteor  paths  is  found  to  be  59.4 
English  miles. 

"  2d.  The  relative  frequency  of  meteors  when  the  heavens 
were  divided  into  eight  equal  parts  was  about  equal  in  all — 
perhaps  a  slight  preponderance  in  the  southeast — and  the 
relative  frequency  in  different  parts  of  the  visible  heavens 
may  be  considered  a  function  of  the  zenith  distance  only. 

"  3d.  Not  quite  one  in  fifty  of  all  the  meteors  seen  at  any 
one  place  should  have  the  middle  points  of  their  apparent 
paths  within  10°  of  the  zenith. 

"4th.  The  number  of  visible  meteors  that  come  into  the 
atmosphere  every  day  would  be  10,460  times  the  number 
visible  at  one  station  ;  or  the  average  number  that  traverse 
the  atmosphere  daily,  that  are  large  enough  to  be  seen  with 
the  naked  eye,  if  the  sun,  moon,  and  clouds  would  permit, 
would  be  30  x  24  x  10,460  =  7,531,000. 

"  5th.  The  number  of  meteoroids  in  the  space  which  the 
earth  traverses  is  discussed  at  length  and  formulae  are  de- 
rived for  computing  the  whole  number  when  the  average 
number  is  known  for  a  given  unit  of  time.  * 

"  6th.  The  average  length  of  the  apparent  paths  derived 
from  213  European  and  803  American  observations  is  12°. 6. 

"  7th.  Adopting  the  theory  that  for  every  meteor  visible  to 

1  Mem.  Nat.  Acad.  Sciences  I,  291. 


PROGRESS  OF    METEORIC  ASTRONOMY   IN  AMERICA.      289 

the  naked  eye  there  are  52.7  that  are  visible  through  a  comet- 
seeker,  the  whole  number  of  meteoroids  coming  daily  into 
the  air  is  400,000,000. 

"  8th.  The  mean  distance  of  the  meteors  from  the  observer 
is  less  than  144  miles. 

"  9th.  The  mean  foreshortening  of  the  meteor  paths  by  per- 
spective is  from  16°.0  to  12°.6. 

"  10th.  The  average  length  of  the  visible  part  of  meteor 
paths  is  between  24  and  40  or  21  and  34  miles ;  probably 
nearer  21  and  34  miles. 

"  llth.  The  mean  duration  of  flight  is  not  much,  if  any, 
greater  than  half  a  second  of  time." 

Prof.  H.  A.  Newton*-  discussed  the  observations  of  the  al- 
titudes of  seventy-eight  meteors  observed  on  November  13-14, 
1863,  at  Washington,  Haverford  College,  Germantown,  Phil- 
adelphia, and  other  points,  giving  diagrams  exhibiting  the 
altitudes  of  these  meteors,  and  also  of  thirty-nine  meteors 
observed  in  August,  18G3,  with  the  following  results :  . 

November  August  me-    - 

meteors.  teors. 

Mean  altitude  at  appearance     .     .  96.2  miles.  69.9  miles. 

Mean  altitude  at  disappearance     .  60.8    "  56.0     " 
Mean  altitude  of  middle  point  of 

path       78.5    "  62.9     " 

In  a  paper  on  "  The  Theory  of  Meteors  "  Pro/.  Daniel  Kirk- 
wood*  arrived  at  the  following  conclusions  : 

"  The  zodiacal  light  is  probably  a  dense  meteoric  ring,  or 
rather,  perhaps,  a  number  of  rings. 

"  Variable  and  temporary  stars  are  caused  by  the  interpo- 
sition of  meteoric  rings. 

"  Mercury's  mean  motion  is  probably  diminished  by  the 
action  of  meteoric  matter. 

"  The  transit  of  a  meteoric  stream  or  cloud  affords  the  most 
probable  explanation  of  the  phenomenon  known  as  '  dark 
days.' 

1  A.  J.  S.,  XL2,  250.  2  Proc.  A.  A.  A.  S.  18G6,  8. 


290  EASTMAN. 

"  It  seems  probable  that  a  ring  of  meteor  asteroids  exists 
within  the  orbit  of  Titan,  Saturn's  largest  satellite,  and 
causes  the  annual  motion  of  the  apsides  of  Titan,  found  by 
Bessel  to  be  30'  28". 

"  Saturn's  rings  are  probably  composed  of  an  indefinite 
number  of  extremely  minute  asteroids  or  meteorites. 

"  The  gaps  in  the  distribution  of  the  mean  distances  of  the 
asteroids  between  Mars  and  Jupiter  are  analogous  to  the 
gaps  in  Saturn's  rings." 

In  May,  1867,  Prof.  Daniel  Kirkwood  published  a  book  l 
under  the  title  "Meteoric  Astronomy,"  designed  by  the 
author  to  present  in  a  popular  form  the  principal  results  of 
observation  and  study  in  that  branch  of  Astronomy.  It 
was  devoted  chiefly  to  the  collection  of  some  of  the  princi- 
pal theories  and  the  more  important  observations,  and  to  pre- 
senting them  in  a  brief  but  popular  form  without  attempt- 
ing to  set  forth  any  new  theory. 

A  paper  by  Prof.  H.  A.  Newton2  in  1867,  "  On  certain  re- 
cent foreign  contributions  to  Astro-meteorology ,"  was  devoted 
to  the  discussion  of  a  table  comparing  the  epochs  and  posi- 
tions of  radiant  points  of  shooting-stars  concluded  inde- 
pendently by  R.  P.  Greg  and  Dr.  E.  Heis;  the  influence  of  the 
August  and  November  meteors  on  the  temperature  of  the 
atmosphere ;  the  paths  and  probable  origin  of  the  shooting- 
stars,  by  Schiaparelli,  and  the  age  of  the  November  group 
of  shooting-stars. 

From  the  data  obtained  from  the  observations  of  the  No- 
vember meteors  in  1867  Prof.  H.  A.  Newton3  discussed  the 
geographical  limits  of  the  shower ;  the  personal  equation  of 
observers ;  the  form  of  the  curve  of  intensity ;  the  breadth 
of  the  radiant  in  latitude;  the  length  of  the  radiant  in  longi- 
tude, and  the  distribution  in  longitude  of  the  perihelia  of 
the  orbits  of  the  meteors. 

1  J.  B.  Lippincott  &  Co.,  Phila.,  18G7,  129  pp. 

2  A.  J.  S.,  XLIII2,  285. 
8  A.  J.  S.,  XLV2,  89. 


PROGRESS  OP   METEORIC  ASTRONOMY   IN  AMERICA.      291 

From  data  obtained  from  the  observations  of  the  Novem- 
ber meteors  of  1867  at  the  U.  S.  Naval  Observatory  and  at 
Richmond,  Va.,  Prof.  S.  Newcomb1,  U.  S.  N.,  computed  the 
altitude  of  nine  meteors,  finding  the  mean  altitude  at  appari- 
tion to  be  102  miles,  and  at  disappearance  47  miles.  From 
data  obtained  from  observations  on  the  same  occasion,  Prof. 
W.  Harknes&y  U.  S.  N.,  discussed  a  method  of  determining 
the  mass  of  such  meteors  as  are  consumed  before  reaching 
the  earth. 

Assuming  that  the  light  produced  is  always  proportional 
to  the  amount  of  material  consumed,  he  arrived  at  the  con- 
clusion that  "  the  mass  of  the  ordinary  shooting-stars  does 
not  differ  greatly  from  one  grain." 

In  1869  a  paper  by  Prof.  Daniel  Kirkwood3  on  "  Comets 
and  Meteors  "  was  devoted  to  exhibiting  the  probable  coin- 
cidences between  the  orbits  of  comets  and  periodical  meteors. 

In  1871  Mr.  Jacob  Ennis*  published  a  paper  entitled  "The 
meteors  and  their  long-enduring  trails." 

The  scope  and  method  of  this  paper  are  briefly  sketched 
by  the  author,  and  are  best  presented  in  his  own  words,  as 
follows : 

"  Firstly,  I  will  bring  forward  many  facts  to  prove  that 
some  meteors  undergo  a  process  of  burning  or  oxidation 
while  passing  through  the  air,  and  that  the  trails  are  the 
smoke  and  ashes  of  such  burning. 

"  Secondly,  I  will  give  facts  and  reasoning  which  show  that 
some  meteors  are  composed  of  various  simple  chemical  ele- 
ments unoxidized,  and  which  are  therefore  capable  of  burn- 
ing in  the  air. 

"  Thirdly,  I  will  show  the  order  and  process  of  creation  by 
which  such  meteors  were  originally  formed  and  left  in  an 
unoxidized  condition. " 

These  points  are  discussed  at  length,  and  numerous  theories 
and  observations  are  cited  as  proof. 

1  A.  J.  S.,  XLV2)  233.  2  A.  J.  S.,  XLV2,  237. 

s  Proc.  Am.  Phil.  Soc.,  XI,  215.  *  Proc.  A.  A.  A.  S.  1871,  122. 

3G—  Bull.  Phil.  Soc.,  Wash.,  Vol.  11. 


292  EASTMAN. 

In  a  paper  on  the  "  Influence  of  meteoric  showers  on  au- 
roras" Prof.  Pliny  K  Chase1  concludes  that  "there  seems 
therefore  good  reason  to  look  for  an  increase  of  auroral  dis- 
plays soon  after  every  meteoric  shower." 

In  discussing  the  meteors  of  November  27,  1872,  Prof.  11. 
A.  Newton*  remarked,  "  With  Professor  Weis  and  others,  I 
am  inclined  to  consider  them  all  to  have  been  once  con- 
nected with  periodic  comets.  The  scattering  took  place  appar- 
ently at  or  near  the  perihelion." 

In  1872  Pro/.  J.  W.  Mallet,  of  the  University  of  Virginia, 
read  a  paper3  on  "  The  occluded  gases  of  meteorites,"  and 
another  paper4  by  this  author  on  the  same  subject  appeared 
in  1875. 

In  1875  Prof.  A.  W.  Wright,  of  Yale  College,  published  an 
account5  of  some  very  carefully  conducted  experiments  made 
to  determine  the  character  and  quantity  of  the  occluded 
gases  of  meteorites. 

From  these  experiments  he  derived  results  differing  ma- 
terially from  those  obtained  by  other  investigators. 

This  paper  was  followed  by  three  others6  during  1875  and 
187G,  in  which  Professor  Wright  reached  the  conclusion  that 
the  spectra  of  gases  from  meteorites  were  identical  with  the 
spectra  of  comets. 

In  a  lecture7  at  the  Sheffield  Scientific  School  of  Yale  Col- 
lege, on  "  The  relation  of  Meteorites  and  Comets,"  Prof.  II. 
A.  Newton,  exhibiting  a  fragment  from  the  meteoric  stone 
which  fell  in  Iowa  February  12,  1875,  very  clearly  presented 
his  theory  of  the  connection  of  these  bodies. 

The  principal  points  in  the  theory,  together  with  some  of 
the  arguments,  may  be  briefly  stated  as  follows : 

Between  the  largest  meteorite  known  and  the  faintest 
shooting-star  that  can  be  seen  on  a  clear  night  with  a  telescope 

1  Proc.  Am.  Phil.  Soc.  XII,  401.  2  A.  J.  S.,  V3,  62. 

3  Proc.  Royal  Society,  XX,  805.  *  A.  J.  S.,  X3,  200. 

5  A.  J.  S.,  IX3,  294.  «A.  J.S.,X3,  44;  XI3,  253 ;  XII3,  105. 

T  Nature,  Vol.  XIX,  315,  340. 


PROGRESS   OP    METEORIC  ASTRONOMY    IN  AMERICA.      293 

there  is  no  essential  difference  as  to  astronomical  character. 
In  all  their  characteristic  phenomena  there  is  a  regular  grada- 
tion of  meteors  from  one  end  of  the  line  to  the  other.  They 
differ  in  bigness,  but  in  their  astronomical  relations  we  can- 
not divide  them  into  groups.  They  are  all  similar  members 
of  the  solar  system.  In  proof  of  these  statements  we  cite 
some  of  the  points  in  which  the  large  and  small  meteors  are 
alike  and  unlike : 

1st.  They  are  all  solid  bodies.  It  is  doubtful  whether  a 
small  gaseous  mass  could  exist  permanently  as  a  separate 
body  in  the  solar  system.  A  liquid  would  probably  freeze 
and  become  solid.  In  any  case,  neither  a  gas  nor  a  liquid 
could  for  an  instant  sustain  the  resisting  pressure  which  a 
meteor  is  subjected  to  in  the  air,  much  less  could  it  travel 
against  it  with  the  velocity  observed  in  ordinary  meteor 
flights.  In  short,  every  shooting-star  must  be  a  solid  body. 

2d.  The  large  meteors  and  the  small  ones  are  seen  at  about 
the  same  height  from  the  earth's  surface.  The  air  is  a  shield 
to  protect  the  earth  from  an  otherwise  intolerable  bombard- , 
ing  by  these  meteors.  Some  of  the  larger  masses  penetrate 
this  shield,  or,  at  least,  are  not  melted  before  their  final  explo- 
sion, when  the  fragments,  their  velocity  all  gone,  fall  quietly 
to  the  ground.  The  small  ones  burn  up  altogether  or  are 
scattered  into  dust. 

3d.  The  velocities  of  the  large  and  the  small  meteors  agree, 
and,  though  they  are  never  measured  directly  very  exactly,  we 
are  sure  that  in  general  they  are  more  than  two  and  less  than 
forty  miles  per  second.  Velocities  of  from  ten  to  forty  miles 
per  second  imply  that  these  masses  are  bodies  that  move 
about  the  sun  as  a  center  or  else  move  through  space.  These 
velocities,  as  well  as  other  facts,  are  utterly  inconsistent  with 
a  permanent  motion  of  such  bodies  about  the  earth  or  with 
a  terrestrial  or  a  lunar  origin. 

4th.  The  motions  of*  the  large  and  small  meteors  as  they 
cross  the  sky  have  no  special  relations  to  the  ecliptic.  If 
either  kind  had  special  relations  to  the  planets,  in  their  origin 
or  in  their  motions,  we  should  have  reason  to  expect  them, 


294  EASTMAN. 

if  not  always,  at  least  in  general,  to  move  across  the  sky 
away  from  the  ecliptic.  The  fact  is  otherwise.  Both  large 
and  small  meteors  are  seen  moving  towards  the  ecliptic  as 
often  as  from  it.  Neither  class  seem,  therefore,  to  have  any 
relation  to  the  planets. 

Again,  in  general  character  the  two  classes  are  alike. 
They  have  like  varieties  of  color ;  they  have  similar  luminous 
trains  behind  them.  In  short,  we  cannot  draw  any  line  divid- 
ing the  stone  or  iron  producing  meteor  from,  the  shooting- 
star,  at  least  in  their  astronomical  relations.  They  are  all 
astronomically  alike.  They  differ  in  size ;  but  that  has  noth- 
ing to  do  with  their  motion  about  the  sun  or  in  space. 

The  general  connection  between  comets  and  meteors  may 
be  exhibited  in  the  peculiar  relations  existing  between  tin- 
meteors  of  November  13-14  and  their  accompanying  comet 
The  orbit  of  these  meteors  is  one  that  is  described  in  153.  •_'."> 
years.  The  meteors  go  out  a  little  further  than  the  planet 
Uranus,  or  about  twenty  times  as  far  as  the  earth  is  from 
the  sun.  While  they  all  describe  nearly  the  same  orbit  tin  y 
are  not  collected  in  one  compact  group.  On  the  contrary, 
they  take  four  or  five  years  to  pass  a  given  place  in  the  orbit, 
and  are  to  bethought  of  as  a  train  several  hundred  millions 
of  miles  long  but  only  a  few  thousands  of  miles  in  thickness. 

Along  with  this  train  of  meteors  travels  a  comet.  It  passi  <  1 
the  place  where  we  meet  the  meteor  stream  nearly  a  year 
before  the  great  shower  of  ISGGancl  two  or  throe  years  before 
the  quite  considerable  displays  of  18G7  and  18G8.  How 
came  it  that  this  comet  and  the  meteors  travel  the  same 
road?  The  plane  of  the  comet's  orbit  might  have  cut  the 
earth's  orbit  to  correspond  with  any  other  day  of  the  year 
than  November  15 ;  or,  cutting  it  at  this  place,  the  comet 
might  have  gone  nearer  to  the  sun  or  farther  away  ;  or, 
satisfying  these  two  conditions,  it  might  have  made  any 
Wangle  from  0°  to  180°  instead  of  467° ;  or,  satisfying  all 
these,  it  might  have  had  any  other  periodic  time  than  33.25 
years ;  even  then  it  might  have  gone  off  in  any  other  direc- 
tion of  the  plane  than  that  in  which  the  ineteoroids  were 


PROGRESS  OF    METEORIC  ASTRONOMY    IN  AMERICA.       295 

traveling.     All  these  things  did  not  happen  by  chance; 
there  is  something  common. 

The  comet  alluded  to  is  not  the  only  one  that  has  an  orbit 
common  with  meteors,  though  it  is  the  only  case  in  which 
the  orbit  of  the  meteors  is  completely  known,  aside  from  our 
knowledge  of  that  of  the  comet.  Every  August,  about  the 
tenth  day,  we  have  an  unusual  number  of  meteors — a  star- 
sprinkle  as  it  has  been  called.  A  comet  whose  period  is 
about  125  years  moves  in  the  plane  and  probably  in  a  like 
orbit  with  these  meteors.  Near  the  first  of  December  there 
have  been  several  star-showers,  notably  one  in  1872,  and 
these  meteors  are  traveling  nearly  in  the  orbit  of  Biela's 
comet.  In  April,  too,  some  showers  have  occurred  which 
are  thought  to  have  had  something  to  do  with  a  known 
comet.  Thus  much  as  to  the  meteors  of  the  star-showers. 
The  sporadic  meteors  are  with  good  reason  presumed  to  be 
(and  observed  facts  prove  some  of  them  to  be)  the  outliers  of 
a  large  number  of  meteor  streams. 

Considering  again  the  November  meteor  stream  and  its 
comet  we  find  that  the  several  bodies  move  along  a  common 
path  not  at  all  by  reason  of  a  present  physical  connection. 
They  are  too  far  apart — in  general,  a  thousand  times  too  far 
apart — to  act  on  each  other  so  much  that  we  may  measure 
the  effect.  Their  connection  has  been  in  the  past.  They 
must  have  had  some  common  history.  Looking  now  at 
the  comets,  we  see  that  they  have  been  apparently  growing 
smaller  at  successive  returns.  Halley's  comet  was  much 
brighter  in  its  earlier  than  in  its  later  approaches  to  the  sun. 
Biela's  comet  has  divided  into  two  or  more  principal  parts, 
and  seems  to  have  entirely  gone  to  pieces.  Several  comets 
have  had  double  or  multiple  nuclei.  In  the  year  1366,  in 
the  week  after  the  star-shower,  a  comet  crossed  the  sky  ex- 
actly in  the  track  of  the  meteors.  A  second  comet  followed 
in  the  same  path  a  week  after.  Both  belonged,  no  doubt, 
to  the  November  stream,  and  one  of  them  may  perhaps  have 
been  the  comet  of  1866. 

The  November  meteor  stream  is  a  long,  thin  one.     We 


296  EASTMAN. 

have  crossed  the  stream  at  many  places  along  a  length  of  a 
thousand  millions  of  miles,  sometimes  in  advance  of  and 
sometimes  behind  the  comet,  and  all  along  this  length  have 
been  found  fragments — sometimes  few,  sometimes  many. 
This  form  of  the  stream  suggests  continuous  action  produc- 
ing it.  A  brief,  violent  action  might  have  given  this  form, 
but  a  slowly  acting  cause  seems  more  natural. 

Again,  in  the  history  of  Biela's  comet  we  have  distinct 
evidence  of  continued  action.  The  comet  divided  into  two 
parts  not  long  before  1845,  and  yet  in  1798  fragments  of  it 
were  met  with  so  far  from  the  comet  that  they  must  have 
left  the  comet  long  before,  probably  many  centuries  ago. 

"  Thus  we  are  led  to  say,  first,  that  the  periodic  meteors 
of  November,  of  August,  of  April,  &c.,  are  caused  by  solid 
fragments  of  certain  known  or  unknown  comets  coming  into 
our  air;  secondly,  that  the  sporadic  meteors,  such  as  we  can 
see  any  clear  night,  are  the  like  fragments  of  other  comets  ; 
thirdly,  that  the  large  fire-balls. are  only  larger  fragments  <>f 
the  same  kind  ;  and,  filially,  that  a  portion  broken  off  from 
one  of  those  large  fragments  in  coming  through  the  air  must 
once  have  been  a  part  of  a  comet" 

"How  came  the  comet  to  break  up?  Perhaps  tin-  prior 
question  would  be,  How  came  the  comet  together?  In  its 
history  there  is  much  that  cannot  yet  be  explained,  much 
about  which  we  can  only  speculate." 

"  Thus,  how  came  this  meteoric  stone  to  have  its  curious 
interior  structure?  As  a  mineral  it  resembles  more  the 
deepest  fire-rocks  than  it  does  the  outer  crust  of  the  earth. 
It  seems  to  have  been  formed  in  some  large  mass,  possibly 
in  one  larger  than  any  of  our  existing  comets.  Some  facts 
show  that  the  comets  have  almost  surely  come  to  us  from 
the  stellar  spaces.  Out  somewhere  in  the  cold  of  space  a 
condensing  mass  furnished  heat  for  the  making  of  this  stone. 
The  surrounding  atmosphere  was  unlike  ours,  since  some  of 
these  minerals  could  hardly  have  been  made  in  the  presence 
of  the  oxygen  of  our  air.  Either  in  cooling  or  by  some  ca- 
tastrophe the  rocky  mass  may  have  been  broken  to  pieces, 


PROGRESS  OF   METEORIC  ASTRONOMY    IN  AMERICA.      297 

so  as  to  enter  the  solar  system  having  little  or  no  cohesion, 
like  a  mass  of  pebbles ;  or  it  may  have  come,  and  probably 
did  come,  a  single  solid  stone. 

In  either  case,  as  it  got  near  to  the  sun  new  and  strong 
forces  acted  on  it. 

The  same  heat  and  repulsion  that  develops  and  drives  off 
from  a  comet  in  one  direction* a  tail,  sometimes  a  hundred 
millions  of  miles  long,  may  have  cracked  off  and  scattered 
in  another  direction  solid  fragments.  One  of  these  contained 
in  it  this  stone,  and  it  wandered  in  its  own  orbit  about  the 
sun,  itself  an  infinitesimal  comet,  how  many  thousands  of 
millions  of  years  we  know  not,  until  three  years  ago  it  came 
crashing  through  the  air  to  the  earth  in  Iowa." 

More  than  ordinary  space  has  been  given  to  the  citations 
from  the  various  statements  and  arguments  and  to  the  con- 
cluding speculation  of  Professor  Newton's  paper  because, 
better  than  any  preceding  American  discussion,  it  presents 
the  status  of  the  modern  theories  of  meteors  and  comets 
which  are  now  generally  accepted  by  the  scientific  world. 

The  latest  formal  discussion  of  this  subject  was  presented 
by  Professor  Newton1  in  his  presidential  address  before  the 
American  Association  for  the  Advancement  of  Science,  at 
Buffalo,  in  1886.  This  address  was  devoted  wholly  to  the 
consideration  of  the  various  theories  in  regard  to  the  motions, 
character,  and  origin  of  meteorites,  meteors,  and  shooting- 
stars. 

The  discussion  in  this  address  follows  the  same  general 
lines  as  in  the  lecture  just  cited,  while  the  various  arguments 
are  presented  with  far  greater  elaboration.  No  new  hypoth- 
eses or  theories  are  offered  ;  but  the  key-note  of  the  address, 
given  in  the  author's  own  words,  is  that  "  science  may  be 
advanced  by  rejecting  bad  hypotheses  as  well  as  by  forming 
good  ones." 

1  Tree.  Am.  Ass.  Ad.  Science  1886,  1. 


298  EASTMAN. 

EXAMINATION  OF  THEORIES. 

The  abstracts  and  excerpts  just  presented  are,  from  the 
limitations  of  the  method  employed,  frequently  very  brief, 
sometimes  disconnected,  and  generally  separated  from  the 
various  discussions  which  led  to  the  results  cited. 

Although  they  present  in  themselves  insufficient  data  for 
an  accurate  study  or  a  rigorous  discussion  of  the  subject, 
they  are  quite  sufficient  to  illustrate  the  evolution  of  the 
modern  theories  as  they  have  been  successively  developed 
from  the  superstitions  and  the  dogmatic  assumptions  of  tin- 
last  century. 

This  development  is  a  fair  illustration  of  the  growth  of 
most  of  the  sciences,  and  the  sometimes  absurd  and  baseless 
theories,  some  of  which  have  been  cited,  are  the  usmd  evi- 
dences of  an  anxious,  persistent  searching  after  the  truth 
which  is  satisfied  only  by  success. 

While  the  modern  theories  have  been  slowly  evolved  from 
a  multitude  of  observations  and  discussions,  expanding  here 
and  there  along  the  lines  of  least  difficulty,  it  is  not  improb- 
able that  frequently  there  has  been  a  lack  of  the  nicest  dis- 
crimination as  to  what  were  real  and  well-established  facts. 

Keeping  in  view  the  precept  that  no  sound  theory  can  be 
based  on  doubtful  data,  it  is  proposed  to  examine  briefly  the 
accumulated  mass  of  so-called  knowledge  of  Meteors  and 
Comets,  with  a  view  to  ascertaining  what  we  actually  know 
about  these  bodies;  what  we  infer,  assume,  and  assert,  and 
to  some  extent,  perhaps,  what  we  do  not  know  about  them. 

METEORS. 

Those  bodies  which  are  usually  designated  as  meteors,  me- 
teorites, and  shooting-stars  are  known,  to  some  extent,  by  every 
intelligent  person.  The  first  name  is  usually  applied  to  those 
sporadic  bodies  which  one  can  see  occasionally  on  any  clear 
night;  the  second  term  is  applied  to  iron  or  stony  musses 
that  sometimes  fall  to  the  earth,  while  the  last  term  is  used 


PROGRESS   OF   METEORIC  ASTRONOMY    IN  AMERICA.       299 

to  designate  those  bodies  which  appear  in  such  periodic 
showers  as  those  of  November  13-14,  August  6-10,  etc.,  but 
which,  like  the  first  named,  are,  almost  without  exception, 
entirely  consumed  before  they  reach  the  earth. 

These  bodies  have  received,  at  various  times,  a  great 
variety  of  names,  such  as  "  Fiery  Tears  of  St.  Lawrence," 
"  Fire-balls,"  "  Bolides,"  "Aerolites/  "  Meteoroids,"  etc.,  most 
of  which  have  been  coined  to  suit  the  fancy  or  ambition  of 
some  aspiring  author.  The  only  definite  knowledge  we  have 
of  this  class  of  bodies  before  they  reach  the  surface  of  the 
earth  is  obtained  with  the  spectroscope,  and  the  results  from 
observations  with  that  instrument  indicate  that  all  these 
bodies  are  similar  in  composition,  and  their  spectra  are  the 
same  as  that  obtained  from  those  masses  that  have  reached 
the  surface  of  the  earth  before  destruction. 

There  appears  to  be,  therefore,  no  reason  for  using  but  two 
names — the  one,  meteor,  for  those  bodies  that  are  consumed 
before  they  reach  the  earth ;  and  the  other,  meteorite,  for  the 
solid  iron  or  stony  substances  that  succeed  in  storming  our 
atmospheric  barriers,  reaching  the  surface  of  the  earth  intact 
and  bringing  our  only  material  messages  from  the  depths 
beyond. 

Sporadic  meteors  as  well  as  meteorites  move  apparently 
in  all  directions.  Meteors  that  appear  in  showers  seem  to 
emanate  from  pretty  well  defined  points  in  the  heavens,  each 
separate  shower  having  its  own  radiant,  and  in  most  cases 
the  bodies  are  not  condensed  in  a  single  compact  mass,  but 
are  scattered  along  the  orbit  in  which  they  move. 

This  orbit  has  been  determined  for  several  of  the  showers 
with  considerable  accuracy. 

From  the  testimony  of  the  meteors  themselves  nothing  is 
known  of  their  origin.  The  theories  of  a  terrestrial  or  a 
lunar  volcanic  origin  are  easily  shown  to  be  absurd,  while 
the  so-called  theories  that  place  their  origin  in  other  por- 
tions of  the  solar  system  are  mere  idle  speculations. 


37-Bull.  Phil.  Soc.,  Wash.,  Vol.  11. 


300  EASTMAN. 


COMETS. 

The  whole  number  of  comets,  real  and  suspected,  from 
about  1770  B.  C.  to  the  end  of  1889  A.  D.,  the  elements  of 
whose  orbits  have  not  been  computed,  is  472.  From  370  B. 
C.  to  the  end  of  1889  A.  D.  the  number  of  comets  the  ele- 
ments of  whose  orbits  have  been  computed  is  309.  Of  these, 
18  are  known  to  have  elliptic  orbits.  In  the  case  of  52,  the 
computed  elliptic  orbits  have  not  been  verified  by  observa- 
tion. 

The  computations  show  that  231  have  parabolic  orbits,  and 
indicate  that  7  have  hyperbolic  orbits. 

Thus  it  appears  that  not  more  than  seven  per  cent,  of  the 
comets  whose  orbits  have  been  discussed  are  known  to  have 5 
elliptic  orbits,  while  it  is  almost  certain  that  seventy-five 
per  cent,  have  parabolic  orbits.  Of  course,  the  periodic 
comets,  whatever  their  origin, belong  now  to  the  solar  system. 

As  it  is  highly  improbable  that  there  are  two  or  more 
kinds  of  comets  of  intrinsically  diverse  character  and  of 
different  origin,  it  follows  that  all  the  comets  had  their 
genesis  beyond  the  limits  of  the  solar  system,  and  that  the 
few  periodic  comets  are  the  exception  to  the  general  law,  and 
at  best  are  only  adopted  members  of  the  solar  family. 

There  are  only  two  sources  of  actual  knowledge  of  the 
physical  constitution  of  comets  : 

One  is  from  the  use  of  the  spectroscope;  the  other  is  the 
behavior  of  the  light  from  a  star  when  seen  through  various 
portions,  but  especially  the  nucleus  of  a  comet. 

As  is  well  known,  observations  with  the  spectroscope  are 
not  always  easily  interpreted,  but  in  this  case  the  difficulty 
is  not  so  great  as  at  first  it  seems  to  be. 

It  is  a  general  law  that  where  there  is  a  continuous  spec- 
trum containing  all  the  primary  colors  without  gaps,  the 
light  is  derived  from  an  incandescent  solid  or  liquid  body. 
A  discontinuous  spectrum  containing  bands  or  bright  lines 
indicates  that  the  light  comes  from  luminous  gases  or  vapors. 


PROGRESS   OF    METEORIC  ASTRONOMY   IN  AMERICA.      301 

To  these  general  rules  there  are  some  important  exceptions 
or  modifications. 

If  the  temperature  of  certain  vapors  or  gases  be  raised  to 
a  high  degree  the  number  and  the  appearance  of  the  colored 
band  or  of  the  bright  lines  change  rapidly,  though  not  uni- 
formly, and  some  investigators  have  asserted  that  if  the 
temperature  be  raised  to  something  over  4,500°  Fah.  the 
spectrum  will  become  practically  continuous.  Similar 
changes  in  the  phenomena  are  observed  if  a  gas,  like  hydro- 
gen, is  rendered  luminous  by  the  electric  spark  and  then 
subjected  to  varying  pressures.  With  a  pressure  amounting 
to  one-twentieth  of  an  inch  of  mercury  the  spectrum  is  dis- 
continuous and  consists  of  several  groups  of  bright  lines  in 
the  green.  As  the  pressure  is  gradually  increased  there  ap- 
pears a  temporary  spectrum  of  bands,  then  a  spectrum  of 
three  lines,  afterwards  a  more  permanent  and  complete 
spectrum  of  bands,  and  finally,  under  a  pressure  of  52  inches 
of  mercury,  a  complete  and  pure  continuous  spectrum. 

The  spectra  of  comets,  which  have  been  obtained  by  care- 
ful and  experienced  observers,  present  a  large  number  of 
variations  and  combinations,  ranging  from  one  or  more 
faint  bands  with  indistinct  or  fluted  borders  against  a  color- 
less background  to  a  faint  continuous  spectrum  with  bands 
or  lines  of  a  greater  or  less  degree  of  brightness  and  defini- 
tion. 

The  most  obvious  interpretation  of  the  spectroscopic  ob- 
servations of  comets  is  that  the  bands  and  lines  are  the  true 
spectra  of  a  gaseous  body,  varying  through  a  wide  range 
under  the  effect  of  changing  pressure  and  temperature,  super- 
imposed upon  the  faint  continuous  spectrum  derived  from 
the  sunlight  reflected  from  the  nucleus  or  other  parts  of  the 
comet. 

Such  is  the  information  derived  from  the  spectroscope. 

In  the  vast  number  of  observations  of  comets,  made  for 
the  determination  of  their  positions  or  their  physical  pecu- 
liarities, it -has  sometimes  been  noted  that  the  comet  passed 


302  EASTMAN. 

between  the  observer  and  a  star  without  diminishing  the 
apparent  brightness  of  the  star  or  changing  its  position. 

While  observing  Comet  I,  1866,  in  January,  1866,  I  saw 
on  one  occasion  the  nucleus  of  the  comet  pass  directly  over 
a  star  of  the  9.2  magnitude  with  no  more  effect  on  the  bright- 
ness of  the  star  than  would  be  produced  by  the  close  prox- 
imity of  any  object  as  bright  as  the  comet's  nucleus.  Similar 
accounts  have  been  given  by  other  observers,  and  the  phe- 
nomenon is  too  well  attested  to  admit  of  a  reasonable  doubt. 

The  light  from  a  star  could  not  pass  unobstructed  through 
a  solid  body  or  a  dense  aggregation  of  solid  bodies;  and, 
considering  this  phenomenon  alone  or  in  connection  witli 
the  appearance  of  the  nucleus  as  it  approaches  and  recedes 
from  perihelion,  it  appears  that  we  are  driven  to  the  conclu- 
sion that  the  nucleus  of  a  comet  is  composed  principally,  if 
not  entirely,  of  gaseous  matter,  which  varies  in  form  ;m<l  in 
density  from  the  effect  of  the  sun's  attraction  and  repulsion. 

COMETS  AND  METEORS. 

The  elements  of  the  orbits  of  four  meteor  streams  have 
been  determined  with  considerable  accuracy.  These  are  (lie 
streams  that  produce  the  showers  of  November  13-1-1,  No- 
vember 27,  April  20,  and  August  10. 

It  has  also  been  found  that  the  orbit  of  the  meteor  stream 
of  November  13-14  coincides  very  closely  with  the  orbit  of 
Comet  I,  1866.  The  orbit  of  the  November  27  stream  corre- 
sponds to  that  of  Biela's  comet,  the  orbit  of  the  April  stream 
to  that  of  comet  I,  1861,  and  the  orbit  of  the  August  stream 
is  nearly  .identical  with  that  of  Comet  III,  1862. 

The  identify  of  these  orbits  is  quite  as  good  as  could  be 
expected  from  the  uncertain  character  of  the  observations 
on  which  the  adopted  positions  of  the  meteor  streams  depend. 

On  these  coincidences  in  the  orbits  of  meteor  streams  and 
of  certain  comets  depends  principally  the  modern  theory 
of  comets  and  meteors,  which,  briefly  stated,  is  as  follows  : 

Sporadic  meteors,  individual  members  of  meteoric  showers, 


PROGRESS  OF    METEORIC  ASTRONOMY    IN  AMERICA.      303 

and  meteorites  differ  in  magnitude  and  appear  under  widely 
varying  conditions,  but  from  an  astronomical  standpoint  they 
are  all  alike. 

They  are  all  solid  bodies  and  are  fragments  of  comets. 

Assuming  that  this  theory  is  true,  we  shall  find  that  some 
of  the  inferences  drawn  from  it  are  of  great  importance  in 
their  bearing  on  cosmical  physics. 

1st.  As  the  meteoric  masses,  both  great  and  small,  are 
derived  from  comets,  they  must  have  originated  beyond  the 
limits  of  the  solar  system,  and  they  furnish  evidence  of  the 
existence  in  space  of  exactly  such  minerals,  though  in  dif- 
ferent combinations,  as  are  found  in  the  earth's  crust. 

2d.  They  arise  from  the  disintegration  of  comets,  which 
for  centuries  have  furnished  the  material  for  the  enormous 
areas  of  bodies  forming  the  various  meteor  streams  that  trail 
along  the  orbits  of  these  masses  for  immense  distances. 

3d.  The  meteors  forming  the  shower  of  November  13-14 
have  been  observed  for  more  than  900  years,  and  yet  the 
comet  whose  gradual  destruction  has  produced  these  bodies 
was  not  discovered  until  1866.  The  August  meteors  have 
been  observed  for  more  than  six  centuries,  but  the  comet 
whose  disintegration  has  furnished  the  material  for  this  va^st 
stream  remains  intact,  and  was  not  discovered  until  1862. 

The  accepted  comet-meteor  theory  does  not  explain  clearly 
the  visibility  of  comets  or  the  changes  that  occur  in  the  ap- 
parent brightness  and  in  the  density  of  the  nucleus  as  these 
bodies  approach  and  recede  from  the  sun ;  neither  does  it 
explain  in  a  satisfactory  manner  the  position  of  the  comets 
in  their  attendant  meteor  streams.  If  comets  are  composed 
of  solid  matter  or  of  discrete  solid  particles,  it  would  seem 
quite  proper  to  ask  why  they  become  visible  at  such  im- 
mense distances  from  the  earth  and  the  sun. 

The  perihelion  distance  of  26  per  cent,  of  the  comets  with 
known  orbits  is  equal  to  or  greater  than  the  mean  distance 
of  the  earth  from  the  sun. 

Many  comets  when  first  seen  are  much  farther  from  the 
sun  than  is  the  earth  at  aphelion,  and  the  spectroscope  only 


304  EASTMAN. 

gives  the  information  that  the  light  is  derived  from  a  gas  or 
vapor.  From  our  constant  experience  with  soli<l  masses  of 
stone  and  iron  on  the  surface  of  the  earth  and  under  the 
unobstructed  influence  of  the  sun,  it  is  impossible  to  sec  how 
the  sun's  heat  alone  can  produce  gas  or  vapor  from  such 
bodies  at  the  observed  distances. 

As  the  comet  approaches  the  sun  the  faint  diffused  mass 
of  the  body  begins  to  contract,  and  a  point  in  the  mass,  gen- 
erally nearer  the  sun  than  the  center,  becomes  brighter  and 
denser,  frequently,  as  it  rapidly  nears  the  sun,  chnnging  its 
form  and  brightness  in  a  marked  manner  from  day  to  day. 

It  is  not  improbable  that  the  solid  constituents  of  mete- 
orites would  be  vaporized  if  they  passed  as  near  the  sun  as 
did  Comet  II,  1882;  but  it  is  not  probable  that  this  change 
does  occur  at  distances  greater  than  the  radius  of  the  earth's 
orbit,  if  it  is  effected  simply  by  the  action  of  the  sun. 

If  the  visibility  is  caused  by  the  assumed  enormous  change 
of  temperature  experienced  by  the  solid  portion  of  the  comet 
in  passing  from  outer  space  to  the  locus  of  visibility  in  the 
solar  system,  then  the  entire  mass  of  the  comet  should  he 
vaporized  and  solid  meteoric  bodies  would  cease  to  exist. 

•If,  on  the  other  hand,  this  visibility  is  brought  about  by 
the  effect  of  this  change  of  temperature  on  the  occluded  gases 
stored  up  in  the  solid  portions  of  the  comet,  then  during  the 
long  period  in  which  these  masses  are  subjected  to  the  solar 
action  these  gases  would  all  be  expelled  and  dissipated  and 
none  would  be  found  in  those  meteorites  which  filially  find 
their  way  to  the  surface  of  the  earth  and  into  the  chemist's 
laboratory. 

The  meteors  of  the  shower  of  November  27  are  scattered 
along  the  orbit  of  that  stream  for  at  least  500  millions  of 
miles.  If  this  elongation  of  the  meteor  stream  is  formed,  as 
is  highly  probable,  by  the  difference  in  velocity  between 
those  meteors  on  that  portion  nearest  the  sun  and  those  on 
the  outside  of  the  mass,  then,  if  the  comet  is  the  meteor-pro- 
ducing body,  the  same  action  would  tend  to  break  it  up  and 
destroy  it  early  in  its  existence  as  a  solar  satellite. 


PROGRESS  OF  METEORIC  ASTRONOMY   IN  AMERICA.      305 

If  the  existence  of  the  comet  as  a  member  of  the  solar  sys- 
tem antedates  the  meteor  stream,  it  is  difficult  to  see  how  the 
comet  could  have  remained  intact  long  enough  to  have  been 
observed,  in  the  presence  of  forces  that  for  thousands  of  years 
have  been  transforming  the  figure  of  the  original  mass  and 
stretching  it  out  into  a  stream  whose  length  is  measured  by 
hundreds  of  millions  of  miles.  It  is  not  improbable  that 
comets  of  large  dimensions  are  destroyed  by  the  action  of 
such  forces ;  but  that  a  body  of  that  character  should  mi- 
raculously survive  its  own  destruction  and  be  found  existing 
in  ordinary  cometary  form  in  the  midst  of  its  own  ruins  is 
a  proposition  that  makes  large  demands  on  the  imagination. 

If  the  brightness  of  comets  is  caused  by  the  vaporization 
of  iron  or  stony  matter,  it  must  be  produced  by  collisions 
between  the  masses  at  such  velocities  that  a  high  tempera- 
ture is  developed,  producing  an  incandescent  vapor  yielding 
a  distinctive  spectrum.  It  seems  difficult  to  explain  how 
such  relative  velocities  can  arise  among  the  individual 
member^  of  the  same  stream  moving  in  a  common  orbit. 
It  is  more  than  probable  that  the  light  of  a  star  passing  from 
the  extremely  low  temperature  of  space  through  the  supposed 
'high  temperature  of  the  comet's  nucleus,  and  again  into  the 
temperature  of  space,  would  suffer  so  much  apparent  change 
of  position  that  it  would  compel  recognition.  It  is  claimed, 
however,  that  the  individual  masses  of  meteoric  matter  which 
form  the  nucleus  are  so  far  separated  that  the  light  of  a  star 
can  pass  through  the  aggregated  mass  without  material 
change  of  direction. 

But  if  the  masses  are  vaporized  by  collisions,  then  there 
must  be  absolute  contact,  which  would  to  a  great  extent 
obstruct  the  passage  of  stellar  light  and  would  be  certain 
to  produce  refraction. 

Lockyer's  Theories. — before  leaving  the  consideration  of 
these  points  I  venture  to  call  attention  for  a  moment  to  a 
recent  theory  which  has  been  set-  forth  with  considerable 
elaboration  of  detail. 


306  EASTMAN. 

In  a  paper  entitled  "  Researches  on  the  Spectra  of  Mete- 
.  orites,"  presented  to  the  Royal  Society  on  October  4,  1887, 
and  in  the  Bakerian  lecture  on  April  12,  1888,  followed  by 
an  appendix  to  the  same  on  January  10,  1889,  Mr.  Lockyer 
presented  in  detail  his  laboratory  experiments,  combined 
with  the  more  or  less  accurate  observations  of  other  astrono- 
mers and  physicists,  which  led  him  to  certain  definite  con- 
clusions in  regard  to  the  relations  of  comets  and  meteors. 

The  author's  conclusions  and  theories  can  be  most  suc- 
cinctly presented  in  the  following  citations  from  the  papers 
mentioned : 

"  The  existing  distinction  between  stars, comets, and  nebu la 
rests  on  no  physical  basis." 

"All  self-luminous  bodies  in  the  celestial  spaces  are  com- 
posed of  meteorites  or  masses  of  meteoric  vapor  produced  I  »y 
heat  brought  about  by  condensation  of  meteor  swan  us  <1  in- 
to gravity.". 

"  Meteorites  are  formed  by  the  condensation  of  vapors 
thrown  off  by  collisions.     The  small  particles  inm-asr  l.y 
fusion  brought  about  again  by  collisions,  and  this  increase 
may  go  on  until  the  .meteorites  may  be  large  enough  t<>  l.e 
^smashed  by  collisions  when  the  heat  of  impact  is  not  suili- 
cient  to  produce  volatilization  of  the  whole  mass." 
f     "  Beginning  with  meteorites  of  average  composition,  the 
extreme  forms,  iron  and  stony,  would  in  time  be  prod  need 
as  the  result  of  collisions." 

"The  spectra  of  all  such  bodies  depend  upon  the  heat  <>f 
meteorites  produced  by  collisions  and  the  average  space  be- 
tween the  meteorites  in  the  swarm,  or,  in  the  case  of  consoli- 
dated swarms,  upon  the  time  which  has  elapsed  since  com- 
plete vaporization." 

"  The  temperature  of  vapors  produced  by  collisions  in 
nebulse,  stars  without  C  and  F,  but  with  other  bright  linos, 
and  in  comets  away  from  perihelion  is  about  that  of  the 
Bunsen  burner." 

"  The  temperature  of  the  vapors  produced  by  collisions 
in  a  Orionis  and  similar  stars  is  about  that  of  the  Bessemer 
flame."  * 


PROGRESS  OF   METEORIC  ASTRONOMY   IN  AMERICA.      307 

"  The  brilliancy  of  the  aggregated  masses  depends  upon 
the  number  of  the  meteorites  and  not  upon  the  intensity  of 
the  light." 

"  The  bright  flutings  of  carbon  in  the  spectra  of  some 
'  stars/  taken  in  conjunction  with  their  absorption  phenom- 
ena, indicate  that  widely  separated  meteorites  at  a  low  tem- 
perature are  involved." 

"  New  stars  are  produced  by  the  clash  of  meteor-swarms, 
the  bright  lines  seen  being  low  temperature  lines  of  those 
elements  in  meteorites  the  spectra  of  which  are  most  brill- 
iant at  a  low  stage  of  heat." 

"A  comet  is  a  swarm  of  meteors  in  company.  Such  a 
swarm  finally  makes  a  continuous  orbit  by  virtue  of  arrested 
velocities.  Impacts  will  break  up  large  stones  and  will 
produce  new  vapors,  which  will  condense  into  small  me- 
teoroids." 

"  When  the  meteorites  are  strongly  heated  in  a  glow-tube 
the  whole  tube,  when  the  electric  current  is  passing,  gives  us 
the  spectrum  of  carbon.  When  a  meteor-swarm  approaches 
the  sun  the  whole  region  of  space  occupied  by  the  meteorites 
*  *  *  gives  us  the  same  spectrum." 

"  The  first  stage  in  the  spectrum  of  a  comet  is  that  in' 
which  there  is  only  the  radiation  of  the  magnesium.  The 
next  is  that  in  which  Mg.  500  is  replaced  wholly  or  par-  < 
tially  by  the  spectrum  of  cool  carbon.  Mg.  is  then  added 
and  cool  carbon  is  replaced  by  hot  carbon.  The  radiation 
of  manganese  558  and  sometimes  lead  546  is  then  added. 
Absorption  phenomena  next  appears,  manganese  558  and 
lead  546  being  indicated  by  thin  masking  effect  upon 
the  citron  band  of  carbon.  The  absorption  band  of  iron  is 
also  sometimes  present  at  this  stage.  ^  At  this  stage  also  the 
group  of  carbon  flutings,  which  I  have  called  carbon  B,  prob- 
ably also  makes  its  appearance.  As  the  temperature  in- 
creases still  further,  magnesium  is  represented  by  b,  and  lines 
of  iron  appear.  This  takes  place  when  the  comet  is  at  or 
near  perihelion." 

"  The  observations  on  meteorites  recorded  in  the  Bakerian 

38— Bull.  Phil.  Soc.,  Wash.,  Vol.11. 


308  EASTMAN. 

Lecture  and  the  discussion  of  cometary  observations  contained 
in  this  Appendix  show  that  the  vapors  which  are  given  out 
by  the  meteorites  as  the  sun  is  approached  are  in  an  ap- 
proximate order :  slight  hydrogen,  slight  carbon  compounds, 
magnesium,  sodium,  manganese,  lead,  and  iron.  Now,  of 
these  the  hydrogen  and  carbon  compounds  are  alone  per- 
manent gases,  and  the  idea  is  that  they  have  been  occluded 
as  such  by  the  meteorites." 

"  The  aurora  being  a  low  temperature  phenomenon,  we 
should  expect  to  find  in  its  spectrum  lines  and  remnants  of 
flutings  seen  in  the  spectra  of  meteorites  at  low  temperatures. 
The  characteristic  line  of  the  aurora  is  the  remnant  of  the 
brightest  manganese  fluting  at  558." 

"  The  spectrum  of  the  nebulre,  except  in  some  cases,  is 
associated  with  a  certain  amount  of  continuous  spectrum, 
and  meteorites  glowing  at  a  low  temperature  would  be  com- 
petent to  give  the  continuous  spectrum  with  its  highest  in- 
tensity in  the  yellow  part  of  the  spectrum." 

"Only  seven  lines  in  all  have  been  recorded  up  to  the 
present  in  the  spectra  of  nebula3,  three  of  which  coincide 
with  lines  in  the  spectrum  of  hydrogen  and  three  corre- 
spond to  lines  in  magnesium.  The  magnesium  lines  rep- 
resented are  the  ultra-violet  low-temperature  line  at  373,  the 
line  at  470,  and  the  remnant  of  the  magnesium  fluting  at 
500,  the  brightest  part  of  the  spectrum  at  the  temperature 
of  the  Bunsen  burner.  The  hydrogen  lines  are  h,  F,  and 
Hf.  (434).  Sometimes  the  500  line  is  seen  alone,  but  it  is 
generally  associated  with  F  and  a  line  a't  495.  The  remain- 
ing lines  do  not  all  appear  in  one  nebulrc,  but  are  associated 
one  by  one  with  the  other  three  lines." 

"  When  a  tube  is  used  in  experiments  to  determine  the 
spectrum  of  meteoric  dust  at  the  lowest  temperature  we  find 
that  the  dust  in  many  cases  gives  a  spectrum  containing  the 
magnesium  fluting  at  500,  which  is  characteristic  of  the 
nebulae  and  is  often  seen  alone  in  them.  If  the  difference  ; 
between  nebulse  and  comets  is  merely  of  cosmographical 
position,  one  being  out  of  the  solar  system  and  one  being  in 


PROGRESS  OF    METEORIC  ASTRONOMY    IN  AMERICA.      309 

it ;  and,  further,  if  the  conditions  as  regards  rest  are  the 
same,  the  spectrum  should  be  the  same,  and  we  ought  to 
find  this  line  in  the  spectrum  of  comets  when  the  swarm 
most  approaches  the  undisturbed  nebulous  condition,  the 
number  of  collisions  being  at  or  near  a  minimum — i.  e.,  when 
the  comet  is  near  aphelion  the  fluting  should  be  visible 
alone." 

After  citing  the  results  of  the  spectroscopic  observations 
of  several  comets,  the  author  remarks :  "  This  spectroscopic 
evidence  is  of  the  strongest,  but  it  does  not  stand  alone. 
Comets  at  aphelion  present  the  telescopic  appearance,  for 
the  most  part,  of  globular  nebulce." 

The  comprehensive  theory  set  forth  in  the  quotations  just 
cited  assumes  that  the  aurorse,  nebulaB,  meteorites,  comets, 
and  most  of  the  stars  all  have  a  common  origin,  and  that 
all  the  multifarious  telescopic  and  spectroscopic  phenomena 
exhibited  by  these  bodies  are  due  to  the  varying  velocities 
of  the  collisions  between  the  meteoric  particles  and  masses 
of  which  in  some  form  all  these  bodies  are  composed. 

We  are  told  that  meteorites  at  a  low  temperature  present 
in  the  spectum  a  certain  line,  at  558,  due  to  manganese,  and 
also  that  this  line  appears  in  the  nebulse,  the  aurora,  and  in 
comets  at  considerable  distances  from  perihelion.  Hence 
the  identity  of  all  these  bodies  is  inferred  and  the  foundation 
of  the  theory  is  laid. 

Meteorites  are  subjected  to  laboratory  experiments  in  tubes 
in  which  the  temperature  is  gradually  raised  to  a  high 
degree  and  the  varying  spectra  is  noted.  Spectroscopic  ob- 
servations of  nebulae,  comets,  and  stars  are  then  compiled 
and  classified,  until  the  several  groups  are  so  arranged  that 
they  present  nearly  the  same 'sequence  of  spectra  that  have 
been  derived  from  meteoric  matter  at  increasing  temperatures 
in  the  experiments. 

The  theory  is  then  extended  and  we  are  given  to  under- 
stand that  when,  in  the  case  of  nebula)  and  stars  greater 
activity  of  collisions  occur,  or  when  a  comet  approaches  the 
sun,  the  same  phenomena  appear  and  in  the  same  order. 


310  EASTMAN. 

The  identity  of  these  bodies  is  then  supposed  to  be  complete 
and  the  theory  established. 

This  theory  of  collisions  rests  upon  a  remarkable  congeries 
ol  experiments,  observations,  and  assumptions.  Many  of  (lit1 
observations  and  many  of  the  laboratory  experiments,  which 
were  made  by  the  author,  as  well  as  much  of  the  data  quoted 
throughout  his  papers  are  entitled  to  the  highest  merit. 
But,  considering  much  of  the  data  and  many  of  the  state- 
ments in  his  conclusions,  and  especially  the  extraordinary 
assertion  that  "  comets  at  aphelion  present  the  telescopic  a  j  >- 
pearance  for  the  most  part  of  globular  nebulrc,"  it  is  not  re- 
markable to  find  the  author's  data,  as  well  as  his  deductions, 
vigorously  attached  by  able  physicists. 

Huggins. —  After  a  careful  study  of  the  spectrum  of  the, 
aurora  Mr.  Huggins1  remarks:  "After  consideration,  I  think 
that  I  ought  to  point  out  that  Mr.  Lockyer's  recent  statement 
that  'the  characteristic  line  of  the  aurora  is  the  remnant  <>f 
the  brightest  manganese  fluting  at  558  '  is  clearly  inadmis- 
sible, considering  the  evidence  we  have  of  the  position  of 
this  line." 

After  a  very  thorough  study  of  the  spectra  of  the  nebula', 
Mr.  Huggins*  writes:  "As,  therefore,  there  seems  to  be  lit  tie 
doubt  that  the  '  remnant  of  the  fluting  at  500'  is  not  coin- 
cident with  the  brightest  nebular  line,  and  the  next  most 
characteristic  group  of  this  spectrum,  the  triplet  at  '57'JO, 
3724,  and  3730,  according  to  Liveing  and  Dcwar,  does  not 
appear  to  be  present  in  the  photographs,  we  may  conclude 
that  the  remarkable  spectrum  of  the  gaseous  nebulae  has  not- 
been  produced  by  burning  magnesium." 

Professor  Liveing3  says  in  regard  to  the  line  denoted  by 
Lockyer  as  470 :  "  I  have  never  seen  the  line  at  A  4703  in  the 
spectrum  of  the  magnesium  flame.  As  it  is  a  conspicuous 
line  in  the  arc  and  spark,  we  looked  for  it  in  the  flame,  but 
did  not  find  it." 


1  Proc.  Roy.  Soc.,  XLV,  435.  2  Proc.  Boy.  Soc.,  XLVI,  55. 

3  Proc.  Boy.  Soc.,  XLVI,  56. 


PROGRESS  OF   METEORIC  ASTRONOMY    IN  AMERICA.      311 

If  the  testimony  of  Huggins  and  of  Liveing  and  Dewar 
represents  the  observed  phenomena,  and  their  observations 
have  not  yet  been  disproved,  then  most  of  the  broad  theories 
of  Lockyer,  which  assume  a  common  origin  and  structure 
for  aurorse,  nebulae,  comets,  and  stars,  lacks  a  basis  of  ob- 
served facts,  resting  wholly,  so  far  as  the  aurora  and  nebulae 
are  concerned,  on  approximate  coincidences  in  the  spectra, 
while  the  assumed  telescopic  appearance  of  cornets  at  aphe- 
lion is  a  creation  of  the  imagination. 

CONCLUSIONS. 

Attention  has  been  called  to  these  various  theories  relat- 
ing to  comets  and  meteors  simply  with  a  view .  to  emphasiz- 
ing the  fact  that  none  of  the  systems,  whether  simple  or 
complex,  seems  to  explain  all  the  observed  phenomena. 

As  a  scientific  explanation,  the  direct  and  simple  is  always 
preferable  to  the  indirect  and  involved  method,  and  this 
safe  precept  should  be  the  guide  in  all  investigations  of  the 
apparent  physical  connection  between  comets  and  meteors. 

It  seems  to  me  that  the  true  theory  of  the  origin  and  the 
relations  of  comets  and  meteors  is  yet  to  be  discovered. 

When  asked  to  give  my  own  theory  of  these  bodies  I  can 
only  reply  that  I  have  none.  At  the  same  time  I  see  less 
objection  to  the  following  hypotheses  than  to  any  of  those 
now  doing  duty  as  theories: 

Meteors  and  meteorites  are  solid  iron  or  stony  bodies  and, 
whatever  their  origin,  are  now  members  of  the  solar  system. 
Comets  are  composed  chiefly  of  gaseous  matter,  and  originate 
outside  of  the  solar  system.  Some  of  these  bodies  on  enter- 
ing the  sphere  of  solar  attraction  are  so  far  drawn  away 
from  their  original  orbits  by  the  masses  of  the  sun's  outer 
satellites  that  they  become  permanent  members  of  the  solar 
system.  Of  these,  at  least  four  have  become  entangled  in 
the  immense  aggregations  known  as  meteor  streams  and 
have  adopted  the  orbits  of  their  captors.  The  meteors  still 
remain  meteors,  however,  and  the  comets  retain  their  former 
identity  and  peculiar  structure. 


312  EASTMAN. 


OBSERVATIONS  OF  METEORS. 

Most  of  the  observers  of  sporadic  meteors  and  meteorites 
have  been  either  amateurs  or  persons  entirely  deficient  in 
that  special  training  which  is  so  essential  in  a  trustworthy 
observer  of  unexpected  phenomena.  Fortunately,  however, 
most  of  the  important  phenomena  have  been  noted  by  in- 
telligent and  skilled  observers,  whose  zeal  and  care  have  left 
little  to  be  desired. 

It  would  be  impracticable  to  mention  even  the  names  of 
all  the  successful  observers,  but  any  sketch  of  the  progress 
of  meteoric  astronomy  in  this  country  would  be  notably  de- 
ficient if  some  of  the  prominent  names  were  omitted. 

The  remarkable  meteor  shower  of  November  13,  1^.".:'., 
attracted  the  attention  of  many  careful  observers  and  /.minus 
students  along  our  Atlantic  coast,  and  for  several  years  the 
subject  was  carefully  investigated  by  Prof.  Dennison  ( )1  in- 
stead and  Prof.  A.  C.  Twining,  who  were  the  pioneers  in  the 
study  of  this  science  in  the  United  States. 

From  1838  when  E.  C.  Herri ck  began  his  work  he  labon-d 
with  untiring  industry  as  an  observer  and  a  compiler  of  ob- 
servations and  other  data  until  his  death,  in  1802,  and  no 
one  in  this  country  did  so  much  as  he  in  promoting  the  ob- 
servation and  investigation  of  the  August  meteors. 

Mr.  Herrick  also  gave  considerable  attention  to  the  study 
and  observation  of  the  November  meteors,  but  this  stream 
was  made  a  special  study  by  Prof.  H.  A.  Newton,  with  tin- 
best  results. 

Professor  Newton's  observations  of  the  November  meteors 
began  in  1860  and  have  been  continued  to  the  present  time, 
while  his  investigations  of  the  motions  and  character  of  this 
stream  place  him  undeniably  at  the  head  of  American 
workers  in  this  branch  of  Astronomy. 

Much  work  of  the  highest  value  was  done  by  Prof.  C.  U. 
Shepard  and  by  Prof.  J.  Lawrence  Smith  in  the  chemical 
examination  of  all  classes  of  meteorites,  and  excellent  in- 


PROGRESS  OF   METEORIC  ASTRONOMY   IN  AMERICA.      313 

vestigations  of  a  similar  character  have  been  carried  out  by 
other  eminent  chemists  in  the  country. 

The  zeal  and  industry  of  Professor  Shepard  was  shown  in 
his  extensive  collection  of  meteoric  specimens,  which  at  the 
time  of  his  death  was  the  largest  in  America. 

The  attempt  to  bring  together  all  the  published  observa- 
tions in  this  country  in  one  systematic  collection  is  a  task 
beset  with  grave  difficulties. 

The  reports  of  these  observations  are  scattered  through  all 
the  scientific  journals,  the  metropolitan  and  local  newspapers, 
and  the  proceedings  of  all  grades  of  learned  societies.  Fre- 
quently the  reports,  when  found,  have  but  little  scientific 
value  from  lack  of  the  necessary  information.  In  many 
instances  much  time  and  space  are  wasted  in  describing 
trivial  details  which  have  no  interest  or  value  in  connection 
with  the  true  meteoric  phenomena,  while  the  really  essential 
data  are  not  mentioned. 

It  sometimes  happens  that  the  only  available  information 
in  regard  to  a  meteorite  is  derived  from  the  report  of  its 
chemical  examination,  and  there  can  be  found  no  astronomi- 
cal data  whatever  to  account  for  its  position ;  it  is  simply  a 
portion  of  the  earth's  surface,  and  the  how,  when,  and  whence 
of  its  advent  remain  unanswered. 

It  has  been  impossible,  sometimes,  to  find  any  trustworthy 
authority  for  essential  data,  and  it  has  been  necessary  fre- 
quently to  interpret  freely  where  the  observer  or  writer  has 
given  but  a  slight  clue  to  his  meaning. 

In  nearly  all  cases  marginal  references  are  made  to  the 
original  papers  in  order  to  facilitate  further  examination,  if 
desired. 

THE  CATALOGUES. 

The  catalogues  of  Sporadic  Meteors,  Meteoric  Showers, 
Observed  Meteorites,  and  Discovered  Meteorites  are  supposed 
to  contain  all  observations,  accompanied  with  the  necessary 
data  that  have  been  found  in  the  various  publications  to 
which  the  author  has  had  access.  It  is  not  assumed,  how- 


314  EASTMAN. 

ever,  that  fhese  lists  contain  all  the  good  observations  that 
have  been  made  in  this  country  ;  in  fact,  it  is  quite  certain 
that  they  do  not,  and  one  of  the  principal  aims  of  this  paper 
will  be  attained  if  this  fact  attracts  sufficient  attention  to 
bring  to  light  the  missing  or  the  unpublished  observations. 

In  all  the  catalogues  the  day  of  the  observation  is  the 
astronomical  day.  It  was  manifestly  impracticable  to  give 
every  reference  to  each  object  in  the  five  catalogues,  and  only 
the  most  important  ones  have  been  retained. 

Occasionally  references  are  only  given  to  the  first  page  of 
a  paper  when  it  contains  several  observations  of  the  sanu- 
phenomenon. 

In  the  reference  notes  at  the  bottom  of  the  page  the  princi- 
pal abbreviated  notation  may  be  explained  as  follows : 

A.  J.  S.,  XXV2,  306,  refers  to  the  American  Journal  of 
Science,  Vol.  XXV,  second  series,  page  306. 

Trans.  A.  P.  S.  refers  to  the  American  Philosophical  Society. 

Proc.  A.  P.  S.  refers  to  the  American  Philosophical  Society. 

Proc.  A.  A.  A.  S.  refers  to  the  proceedings  of  the  American 
Association  for  the  Advancement  of  Science. 


CATALOGUES 


i.-v. 


316 


EASTMAN. 


CA.TA.LOGMJK    I. 


Number. 

DATE. 

Locality. 

Iron  or  stone. 

Year. 

1781(?) 

1807 
1810 
1823 
1825 
1827 
1828 
1829 
1829 
1835 
1837 
1839 
1840 
1843 
1844 

1846 

1847 
1848 
1849 
1855 
1857 
1857 
1859 
1859 
1859 
1860 
1865 
1868 
1868 
18H9 
1871 
1874 
1875 
1876 
1876 
1877 
1877 
1879 
1879 
1883 
1885 
1886 
1887 
1890 

Month. 

Day. 

Hour.  Min. 

1 

2 
3 
4 

5 
6 
7 
8 
9 
10 
11 
12 
13 
14 
15 

16 

17 

18 
19 
20 
21 
22 
23 
24 
25 
26 
27 
28 
29 
30 
31 
32 
33 
34 
35 
36 
37 
38 
39 
40 
41 
42 
43 
44 

Portage  Bay,  Chilcot  Inlet,  Alaska  

OD 

L  a:  x  x  ~  x  x  -f.  x  -i.  x  x  x  x  x  x  x  x  x  x  x  x  x  —  x  x  x  x  -  x  x  x  x  x  x  x  x  r-i 

December  

13 
30 

18.5 

Caswell  N  C   

August 

7 

10 

May           

9 

8umner  Co.,  Tenn  

4 

May  

8 
15 

3 

Forsyth  Co    Ga         

Deal    N  J 

July 

30 
5 
13 

2 
3 
3 

Charlotte,  Dickson  Co.,Tenn  

May  

Little  Piney  Pulaski  Co.,  Mo  

March 

25 

Argentine  Republic                        . 

August 

14 

25 
19 
31 
5 
1 

3 

3 
16 
3 
3 

Cape  Girardeau    Mo              

February 

May 

Castine  Me 

October  
August 

Charlotte,  Cabarrus  Co  .  N.  C  

Lincoln  Co    Tenn 

April  

Cor-ta  Rica,  Central  America     

Independence  Co.,  Iowa  
Harrison  Co.,  Ind  

March  
July  
August..  '.  
May        

28 
4 
11 
1 
24 
27 
5 
5 
20 
14 
12 
24 
21 
2 

4 

21 
5 
3 
23 

20 
2.5 
10.5 
21 
8.75 

Crawford  Co.,  Ark  
Bethlehem,  N.  Y  
New  Concord,  Ohio  
Vernon  Co.,  Wis  

March  

November  
December  
October  
May  
May  

Danville,  Ala  

Frankfort,  Ala  

Stewart  Co.,  <-ia  .    ... 

Searsmont,  Me 

Nash  Co.,  N.  C  

February  
June  
December  

Iowa  Co.,  Iowa 

Kansas  City,  Mo  

Rochester,  Fulton  Co.,  Ind  
Warrenton    Warren  Co    Mo 

23 

Cynthiana,  Harrison  (Jo.,  Ky....v  

May  

10 

5 

Fomatlan  Jalisco  Mexico 

Calderilla  Chili 

1 
1 

I 
S 

s 

November  
March  
January  
May  

27 
27 
21 
2 

3  
2 
5        15 

Mazapil,  Mexico  

Johnson  Co.,  Ark 

De  Cewsville,  Huldirnand  Co.,  Ontario  
Winnebago  Co.,  Iowa      .     . 

1.  Cat.  State  Mining  Bureau  of  Cal.,  1888,  No.  2925. 

,  f  Trans.  Amer.  Phil.  Soc.  VI,,  323. 

2-  \A.  J.  S.  XXXVIIj,  130;  VI2,410. 

3.  A.  J.  S.  Ho,  392. 

4.  A.  J.  S.  Vf  li,  170;  IX,,  400. 

5.  A.  J.  S.  I  Xlt  351  ;  Xlf  131  :  VL,,  406. 
G.  A.  J.  S.  XVII,,  326;  XVIII,,  200,378. 

7.  A.  J.  S.  XV!,  195;  XVIlt  191. 

8.  A.  J.  S.  XVII I,,  388. 

9.  Proc.  A.  A.  A.  S.,  1851,  Vol.  II,  188. 

10.  A.  J.  S.  XLIXa,  336. 

11.  A.  J.  S.  XXXII,,  395. 

12.  A.  J.  S.  XXXVlIj,  385;  XXXIXlf  254. 

13.  A.  ,).S.  IV2,  353;  VI2,  416. 

14.  A.  J.  S.  II2,  392;  VI2,  411. 

15.  Proc.  Lit.  and  Phil.'Soc.  Liverpool,  VII,  18.™. 

16.  A.  J.S.  XXXII3,  229. 

17.  A.  J.  S.  IV2,  288,  429. 

18.  A.  J.S.  VI2,  251,400. 

19.  A.  J.S.  IXo,  143;  Xo,  127. 

20.  A.  J.  S.  XXIVo,  134";  XXXL>,  2fi4. 

21.  Buchner,  93. 

22.  A.  J.  S.  XXXo,  208. 


PROGRESS   OF   METEORIC   ASTRONOMY   IN   AMERICA. 
Observed.    Meteorites. 


317 


Number. 

Weight. 

Authority. 

Remarks. 

l 

88       Ibs 

Seen  to  fall  by  the  father  of  one  of  the  oldest 

2 
3 

4 
5 

c> 
7 
8 
0 

300         " 
3          " 
4          " 
16.5      " 
11 
4          " 
36          " 

Nathan  Wheeler  
Madison. 
A.  Dinsmoor. 
W.  D.  Harrison. 

Elias  Beall. 

Indians. 
Observed  by  many  persons. 

« 
Weight  "  rather  more  than  half  an  ounce." 

10 

9       Ibs 

G   Troost 

11 

12 
13 

0.5    Ib. 
50       Ibs. 

Mr.  Harrison. 

Weight  370.5  grains. 

14 

lr> 

13       Ibs. 

0.  U.Shepard. 

Fall  witnessed  by  1,400  soldiers.    About  a  cubic 

it; 

17 

is 

1!) 

20 
2] 

•>•> 

4.5    Ibs.   | 

130      Ibs. 
0.1    Ib. 
19.5    Ibs. 
3.9      " 

E.  8.  Dana. 
S.  L.  Penfield. 
D.  C.  Rogers. 
Giles  Gardner. 
H.  Bost. 
James  B.  Dooley. 

C.  U.  Shepard  

yard  of  the  mass  remained  above  the  surface 
of  the  ground. 

Fell  in  the  "summer"  of  1857. 

23 

3  7    Ibs 

Several  observers. 

"1 

Mr.  Scott. 

28 

(J.  U.  Shepard  

"Smaller  than  a  pigeon's  egg." 

2(1 

"7 

400.2    Ibs. 

J.  L.  Smith. 

28 

'.!!) 
80 
31 
Rj 

'>'? 

4.5    Ibs. 
1.7      " 
0.8    Ib. 
12       Ibs. 

500       Ibs 

W.  Brown. 
Jas.  W.  Hooper. 
Mrs.  Buck. 

Many  observers. 

SI 

:55 
36 

'17 

0.8   Ib. 
100       Ibs. 
15         *' 

A.  J.  Morris. 

» 
"Fell  in  the  afternoon." 

:is 
'>'> 

750         " 

O  U  Shepard  

Several  pieces  ;  the  largest  weighed  about  2  Ibs. 

"  Small  " 

Ward  and  Howell  

Not  yet  described. 

11 
42 
43 

8.7    Ibs. 
107.5      " 
0.75  Ib. 

W.  B.  Hidden. 
G.  F.  Kunz;. 
E.  E.  Howell. 
G  F  Kunz 

Probably  more  fragments  to  be  discovered. 

23.  A.  J.  S.  XXVIII2,409. 

24  Owens'  2d  Geolog.  Reconnaissance  of  Arkansas,  408. 

25.  A.  J.  S.  XXXo,  206. 

/A.  . I.  S.  XX Xo  103,  207,  206; 

26<  I  A.  J.  S.  XXXlo,  87 ;  XXX1I2,  30. 

27.  A.  J.  S.  XII3,  207.   * 

28.  A.  J.  S.  XI,  1X2,  90. 

29.  A.  J.  S.  XLVIir2,  240. 

30.  A.  J.  S.  L2,  335,  339. 

31.  A.  . I.  S.I  1 3,  133,200. 

32.  A.  J.  S.  X3,  147. 

33.  A.  J.  S.  1X3,  407,  459  ;  X3,  44,  357. 

34.  A.  J.  S.  XI I3,  316. 

35.  A.  J.S.  XII I3,  207,243. 

36.  A.  J.  8*  XIII*  243;  XIV3,219. 

37.  A.  J.  S.  XI113,  243;  XI V3,  219. 

38.  A.  J.  S.  XVIII3,  77, 186;  XIX3,  459,495;  XX3,  136. 

39.  A.  J.  S.  XXX3, 105. 
40. 

41.  A.  J.  S.  XXXIII3,  221. 

42.  A.  J.  S.  XXXIII3,  494,  500. 

43  Science,  N.  Y.,  March  7, 1890, 167. 

44.  Science,  N.  Y.,  May  16, 1890,  304. 


318 


EASTMAN. 


II.- 


Number. 

DATE. 

Locality. 

Iron  or  stone. 

Year. 

Month  and  day. 

1 

2 
3 
4 
5« 
ti 
7 
8 
9 
10 
11 
12 
13 
14 
15 
16 
17 
18 
19 
20 
21 
22 
23 
24 
25 
26 
27 
28 
*9 
30 
31 
32 
33 
34 
35 
36 
37 
38 
39 
40 
41 
4'2 
43 
44 
45 
46 
47 
48 
49 
50 
51 
52 
53 
54 

1735 

1784 
1792 
1808 
1810 
1811 
1818 
1819 
1820 
1822 
1826-7 
1828 
1832 
1834 
1834 
1835 
1836 
1839 
1839 
1840 
1840 
1840 
1841 
1842 
1842 
,1842 
1842 
1845 
1845 
1846 
1846 
1847 
1847-8 
1849 
1850 
1850 
1850 
18  0 
1853 
1853 
1853 
18A3 
1854 
1854 
1855 
18P6 
ISf.li 
1856 
1856 
1856 
1856 
1856 
1857 
1858 

1. 
1. 
I. 
I. 
I. 
I. 
I. 
1. 
I. 
I. 
1. 
I. 
I. 
I. 

i! 

i. 

i 

i. 

i. 

i! 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
i. 
j. 
i. 

L 

l. 
I. 
I. 
I. 
I. 
I. 
I. 
I. 
I. 

Hahia  Brazil                                  

Red  River,  Texas               

Durango  Mexico  

Lock  port  N   Y 

Burlington,  N.  Y  
Guilford  Co    N   C                          . 

Waterloo  Seneca  Co    N  Y  

Bedford  Co    Pa 

Walker  Co.  Ala.                .     . 

Scriba  Oswego  Co    N  Y 

Claiborne  Clark  Co    Ala 

Buncombe  Co    N  C 

Brazo»<  Texas 

March    

Putnam  Co    Ga 

Buncombe  Co.,  N.  C  
Chili  

February  26  

Cocke  Co    Tenn 

Smithland,  Livingston  Co.,  Ky  

February  

Lexington  Co.,  S  C 

Roanoke  Co.,  Va  

Carthage  Tenn 

Green  Co.,  Tenn 

DeKalb  Co.,  Tenn  
Otsego  Co.,  N.  Y.  ..             

» 

Franconia  N  H 

*.'.'.'.'.*.".!."'.'.'.".!!!!'.!'.'.!!'. 

Jackson  Co.,  Tenn......  
Chesterville,  S.  C  
Murfreesborough,  Tenn  

Pittsburgh   Pa 

Allegheny  Co.,  Pa  

Seneca  River,  N.  Y. 

Salt  River  Ky 

Botetourt  Co.,  Va  

Jefferson  Co    Tenn 

Union  Co.,  Ga  

July  

Campbell  Co.,  Tenn  
Tazewell,  Claiborne  Co.,  Tenn. 

August  

Madoc,  Ontario  

Haywood  Co.,  N.  C  

Coahuila,  Mexico  

Nelson  Co.  Ky 

Nebraska  

Madison  Co.  N  C 

Kor^vth   Tanev  Co    Mo 



Marshall  Co.,  Ky....'.  
Denton  Co.,  Texas  

Oktibbeha,  Miss  

Laurens  Co     S  C 

Washington  Co.,  Wis  ..'.  

1. 

2. 

3. 

4. 

0. 

6. 

7. 
S. 
9. 
10. 
11. 

("Smithsonian  Report  1863,  55,  85. 
t  A.  J.  8.  XVIII2,  3fi9  ;  XIX2,  161,  162. 
JA.J.S.  XV2,12;  XXXVI3",158. 
\Sci.  Am.  Supp.  Oct.  19,  1889. 
A.  J.  S.  XV2,  11. 
A.  J.  S.  VIII,,  218;  XVIi,  217;  XXVII,   382 
A.  J.  S.  XVo,  11. 
A.  J.  S.  XV2,  19. 
A.  J.  S.  XLVIIL.,  388;  II2,  374,  391. 
A.  J.  S.  XLVJj,  401  ;  Ho,  391  ;  XVo,  20. 
A.  J.  S.  XVIIi,  140  ;  XL,,  369. 
A.  J.  S.  XVIIi,  140;   II2.  391;  XVo,  21. 
A.  J.  S.  XI2)  39  ;  XXX1V2,  298.     " 

15.   A.  J.S.  XXXIV!,  332;  XLVIII^HS. 
16.   A.  J.  S.  XXXVl!,  81;  XLIlIi,359. 
17.   A.  J.S.  XXX  I2,  459. 
18.   A.  J.  H.  XVII2,  331. 
19.    A.  J.S.  IVo,  82. 
20.   Lon.,  Ed.  and  Dublin  Phil.  Mag.  X4, 
21.   A.  J.S.  XXXVII  I1(  250;  XLIIli,  351. 
22.   A.  J.  8.  II2,357;   XV«,  21. 
(A.  J.S.  X2,  128;  X"Vo,  5,  16. 
23.    -1  Proc.  A.  A.  A.  S.  1850,  Vol.  I,  152 
^     Vol.  11,189. 
24.    A.  J.S.  XLIIIx,  lf,9;  Uo,  392. 
25     A   J   8   X  LI  IIj   1  (',')•   H."   W 

12. 
;  185 

12. 
13. 
14. 

A.  J.S.  II2,  391;  XVo,  21. 
A.  J.  S.  XLIXj,  344  ;"II2,  391  ;  XV2)  21. 
A.  J.  S.  XLi,  366  ;  1I2,  390  ;  IVa,  75. 

26.    A.  J.  8.  Ho,  350  ;  XV2,  '20. 
27.   A.  J.  S.  XLIXi,  342  ;  "lL>,  391. 

PROGRESS   OF    METEORIC    ASTRONOMY    IN    AMERICA. 
Discovered.    ^Meteorites.. 


319 


Number. 

Weight. 

Authority. 

Remarks. 

1 
g 

1,400   Ibs. 
11  819       " 

Jo8eph  Henry  

The  "Ainsa  "  or  "  Tucson  "  meteorite. 
The  "  Bendego"  meteorite 

a 

4 
5 
6 

2,000       " 
1,635       " 
1,700       " 

Weight  30,000  or  40  000  Ibs 

7 
8 
9 

10 

11 
12 

36    Ibs. 
IfiO       " 
28       " 
2       " 
0.1  lb. 

B.  Silliman. 
B.  Silliman. 
C.  U.  Shepard. 
C.  U.  Shepard. 
C.  U.  Shepard  
C  U  Shepard 

Rammelsburg  thought  this  was  not  a  meteorite. 

13 
14 

if, 

n 

17 
18 
I'.t 
20 
21 
22 
2:5 
"4 

165    Ibs. 
8       " 
40      " 
30       " 
324      " 
72      " 
1.3   " 
17      " 
2,000      " 
9.9  " 
117      " 

G.  Troost. 
C.  U.  Shepard. 
C.  T.  Jackson. 
C.  U.  Shepard  
C.  U.  Shepard. 
.1.  E.  Willett. 
C.  U.  Shepard. 
R.  P.Greg  
G.  Troost. 
G.  Troost. 
0.  U.  Shepard  
J  B.  Rogers 

One  date  given  is  1845. 

Found  in  the  desert  of  Tarapaca. 

Found  on  "Ruff's  Mountain." 
"  Original  mass  of  many  pounds'  weight  " 

26 

W   B  Rogers 

20 

27 
28 
•"1 

280    Ibs. 
29       " 
36       " 

G.  Troost. 
G.  Troost  

G.  Troost. 
C  U  Shepard 

Found  near  Babb's  mill. 
Weighed  276  grains 

uu 

Weighed  "  15  or  20  pounds  "     ** 

''ll 

G  Troost 

Weighed  15  oz 

32 

:« 
34 
3S 

•',[; 

36    Ibs. 
19       " 
0.6  lb. 
292     Ibs. 
9       " 

C.  U.  Shepard. 
G.  Troost. 
F.  A.  Genth. 
B.  Silliman. 

Date  somewhat  doubtful 

87 

••is 

8      " 

B.  Silliman. 
C.  U  Shepard 

Original  mass  lost 

15'.) 

40 
41 

4-J 

4:5 
44 

2.5  Ibs. 
15       " 
0.3  lb. 
60     Ibs. 
370       " 

C.  U.  Shepard  
T.  Sterry  Hunt. 
C.  U.  Shepard.      .. 

Also  described  by  J.  L.  Smith. 
Weight  about  ^  oz. 

40 

252    Ibs 

J  L  Smith 

The  "Couch"  meteorite 

46 

47 

48 

4y 

.r.o 
r>i 

0.2  lb. 
35    Ibs. 
0.1  Ib. 
1!»7    Ibs. 
15      " 

G.  J.  Brush. 

G.  J.  Brush. 
C.  U.  Shepard. 
C.  U.  Shepard. 
C  U  Shepard 

Weighed  66  grains. 

63 

53 
54 

0.3  Ibs. 
4.7   " 
85.8   " 

W.J.Taylor  
W.  E.  Hidden. 
F.  Breundecke. 

Found  in  an  Indian  mound. 

• 

A.J.S.  XLIXX,  341;  II2,  391. 

A.  J.S.  II2.  391;  XV2,  16. 

A.  J.S.  Ho,  392;  IVo"  87. 

A.  J.S.  IIo",357;  XVo,  21. 

A.  J.S.  VIlo,  449;  XVo,  21. 

A.  J.S.  V2.  351;  XV2,  21. 

A.J.S.  XVo,22;  XI I3,  72. 

A.  J.  S.  XVo,  7  ;  Proc.  A.  A.  A.  S.  1850,  Vol. 

11,37. 

A.  J.  S.  XIV2,  439  ;  XV2,  363. 
A.  J.  S.  XV2,  22  ;  Proc.  A.  A.  A.  S.  1850,  36. 
A.  J.  S.  XLLI2,  250. 
A.J.S.  XVII2,329. 
A.J.S.  XVII2,  328. 
A.  J.  S.  XIXo,  153. 


42.  A.  J.  S.  XVIIo,  131,  325 ;  XI X2, 153. 

43.  A.J.S.  XIXo,"  417, 

44.  A.J.S.  XVlf.,,327. 

4,  ?  A.J.S.  xiXj,  160. 

40>  t  Smithsonian  Report.  1863,  56. 

46.  A.  J.  S.  XXX2,  240  ;  XXXI2,  459. 

47.  A.  J.  S.  XXXo,  204;  XXXIIo,  146. 

48.  A.J.S.  XXX2,  240;  XXXIo,  459, 

49.  A.  J.  S.  XXX2,  205;  XXX I V3.  467. 

50.  A.  J.  S.,  XXX2,  240  ;  XXXIo,  459. 
,,  /A.  J.S.  XXX I2,  459. 

0       ( Trans.  St.  Louis  Acad.  Sci.  I,  623. 

52.  A.J.S.  XX I  Vo,  293. 

53.  A.  J.  S-.  XXX I3, 463. 

54.  Smithsonian  Report  1869,  417. 


320 


EASTMAN. 


1 1  ,-r>is- 


DATE. 

. 

stone. 

Numbe 

Year. 

Month  and  day. 

Locality. 

Iron  or 

55 

1858—9 

57 

1860 

Mountains  of  East  Tennessee  

58 

1860 

Franklin  Co.,  Ky  

59 

1860 

October 

1860 

61 

1860 

62 

1863 

Rensselaer  Co    NY       .        .                   

63 

1863 

February  18    .  .. 

Colorado 

64 

1863 

Tucson    Arizona                

1863 

Dakota 

66 

1866 

Bear  Creek  Colo                  

67 

1866 

Frankfort    Ky 

68 

1867 

Allen  County  Ky  

69 

1868 

April 

Losttown   Cherokee  Co    Ga 

70 

1868 

44  Southeastern  Missouri  "  

7t 

1868 

Auburn   Macon  Co    Ala 

72 

1869 

71 

1869 

El  Dorado  Co     Cal 

74 

1869 

Trenton   Wi*» 

7*> 

1870 

Howard  Co    Ind  ... 

76 

1873 

August 

Madison  Co    N  C 

77 

1873 

Cleburne  Co.  Ala  .   . 

78 

1874 

79 

1875 

- 

San  Francisco   Brazil  

80 

1877 

Whitfield  Co    Ga. 

81 

1878 

Fayette  Co.,  Texas  

82 

1879 

Whitfield  Co   Ga 

83 

1879 

July  10  

Davidson  Co  ,  N.  C. 

84 

1879 

I  van  pah  Cal 

85 

1880 

Eagle  Station,  Carroll  Co    Ky 

86 

1880 

Lexington  Co    S  C     . 

87 

1880 

Rutherford  Co..  N.  C  

88 

1882- 

June  10  

Maverick  Co    Texas 

89 

1882 

Burke  Co.,  N.  C  

<><) 

1883 

May  15  

Grand  Rapids  Mich 

y] 

1883 

Little  Miami  Valley,  Ohio.  .  .             .     . 

Otf 

188.3 

Wayne  Co.,  W.  Va  

93 

1884 

June  

Independence  Co.,  Ark. 

•14 

1884 

Hammond,  St.  Croix  Co.,  \Vis  .... 

<>5 

1884 

August  

Santa  F6  County,  New  Mexico 

96 

1884 

Chili  

97 

1885 

Catorze,  San  Luis  Potosi,  Mex 

98 

1887 

January  

Laramie  Co    Wyoming 

99 

1887 

March  

Claiborne  Co   Tenn 

TOO 

1887 

March  

Cumberland  Co.,  Tenn 

101 

1887 

March  27  

Chattooga  Co    Ga 

10'} 

1888 

April  30  

Welland,  Ontario  .. 

* 

103 

1888 

Chili.... 

104 

1888 

Chili.... 

I      S 

105 

1888 

Chili  

106 

1888 



Hamilton  Co.,  Texas.. 

55.  A.  J.  S.  XV3,  337. 

56.  Pmo.  Boston  Soc.  Nat.  Hist.  Vol.  7, 161, 174, 

175,  191,  279.  289. 

,7  fA.  J.S.,  XXXI V3,  473. 

'•  \  Proc.  Acad.  Nat.  Sci.  Phil.  1886,  366. 

58.  Smith.  Report  1868, 343;  A.  J.S.  XLIX.331. 

59.  A.  J.  S.  XXX To,  151,  265. 

60.  A.  J.  S.  XXXI*  151,  266. 

61.  A.  J.S.  XL,,  21 3;  XXXIV3,  471. 

62.  A.  J.  S.  XX'XIV3,  60. 

63.  A.  J.  S.  XLIIo.  218. 

M  ?A.  J.S.  XXXV I8, 152. 

•  (  Proc.  Cal.  Acad.  Sci.  Ill,  30. 


65.  A.  J.  S.  XXX VI2,  259. 

66.  A.  J.S.  XLI12,  250,280;   X 


XLIII2,280. 


67.  A.  J.S.  XLIXo,  331. 

68.  A.  J.  S.  XXXIII»,  500. 

69.  A.  J.  S.  X  LVf.,,  257  ;  XLVIL,,  234. 

70.  A.  J.  S.  XLVllo,  233. 

71.  A.  J.  S.  XLVII,,  230. 

72.  A.J.  S.  XXX If,,  226. 

73.  A.J.  S.  IIIo,  438;  VI3,  18. 

74.  A.  J.  S.  XLVIIo,  271  ;  III3,69. 

75.  A.  J.  S.  V3,  155  ;  VI L,  391. 

76.  A.  J.S.  XI  I,.  439. 

77.  A.  J.S.  XIX,.  370;  XX3,  74. 

78.  A.J.  S.  XI3,  473;  XIII3,  211. 

(Comptes    Rendus    LXXXIH,  917,  918 

79.  <      LXXXIV,  478,  482, 1085,  1508. 

(A.  J.  S.  XXlIIg,  232 ;  XXIX3,  33,  490. 


PROGRESS   OF    METEORIC   ASTRONOMY   IN    AMERICA, 
covered.    Meteorites— Cont'ci. 


321 


1  Number. 

Weight. 

Authority. 

Remarks. 

M 

152    Ibs. 

J.  W.  Mallet. 

ft 

John  Evans  

J^Jass  above  ground  45x35  feot 

67 

254    Ibs. 

F.  A.  Genth. 

68 

0.1  Ib. 

G.  J.  Brush. 

61 

112    Ibs. 

Found  by  Wm.  Daring. 

ft 

37      " 

Found  by  D.  Crockett. 

01 

BS 

3.3  Ibs."" 

J.  L.  Smith  
S.  C.  H.  Bailey. 

Specimen  weighed  22%  oz. 

ft 

29       " 

Found  near  Central  City  by  Otho  Curtice 

(i4 

632      " 

(if 

10.G   " 

Dr.  Jackson 

Found  in  the  u  Dakota  Indian  country  J1 

64 

436      " 

J.  L.  Wilson. 

67 

24      " 

J.  L.  Smith. 

(i,S 

24.3   " 

J.  E.  Whitfield. 

*;r 

6.6   " 

7< 

0.8  Ib. 

C.  IT.  Shepard. 

71 

8    Ibs. 

0.  U.  Shepard. 

7S 

1.9   " 

E.  S.  Dana. 

7:5 

85       " 

B.  Silliman. 

74 

143.5   "' 

J.  L.  Smith  . 

Six  fragments  found*  the  first  in  1869 

75 

4      " 

E.  T  Cox. 

7  c; 

25      " 

B.  S.  Burton. 

77 

35.8   " 

W.  E.  Hidden. 

78 

IK)      " 

C.  U.  Shepard. 

78 

Nil 

22,048       " 
13      " 

E.  Guignet  
W.  E.  Hidden. 

In  the  province  of  San  Catherina. 

81 

321       " 

Whitfield     and 

Merrill. 

82 

'117      " 

C.  U.  Shepard. 

83 

2.8   " 

W.  E.  Hidden. 

84 

128.2   " 

C.  U.  Shepard. 

85 

80      " 

G.  F.  Kunz. 

80 

10.5   " 

C.  U.  Shepard. 

87 

4.8    " 

L.  G.  Eakins. 

88 

97.25  " 

W.  E.  Hidden. 

89 

1     tt>. 

G.  F.  Kunz. 

90 

114    Ibs. 

J.  R.  Eastman. 

1)1 

G.  F.  Kunz  

Fragments  found  in  mounds  by  F.  W.  Putnam  ;  now  in 

the  Peabody  Museum. 

92 

26    Ibs. 

G.  F.  Kunz  

Several  fragments. 

!K5 

94      " 

W.  E.  Hidden. 

94 

53       " 

Davenport  Fisher. 

95 

324.4   " 

G.  F.  Kunz.  ... 

Several  fragments. 

96 
97 

14.5   " 
92      " 

Ward  and  Howell. 
G.  F.  Kunz. 

Found  near  Puquios.    Not  yet  described. 

98 

25.06  " 

G.  F.  Kunz. 

99 

18      " 

G.  F.  Kunz. 

00 

94.5   " 

J.  E.  Whitfield. 

01 

27       " 

G.  F.  Kunz. 

02 

E.  E.  Howell. 

03 
04 

or. 

16      " 

27      " 

Ward  and  Howell. 
Ward  and  Howell. 
Ward  and  Howell. 

Thirty  leagues  east  of  Taltal.    Not  yet  described. 
Thirty-five  leagues  S.  E.  of  Taltal.    Not  yet  described. 
Estimated  at  from  6  to  8  Ibs. 

00 

179       " 

Ward  and  Howell. 

Found  five  miles  south  of  Carlton.    Not  yet  described. 

80.   A.  J.  S.  XIV3,  246;  XXI3,  286. 
81.   A.  J.  S.  XXXVI3,  113. 
82.   A.  J.  S.  XXVI3,  336;   XXXIV3,  473. 
8S.   A.  J.  S.  XX3,  3*4. 
84.   A.  J.  S.  XIX3,  381. 
85.   A.  J.  S.  XXXIIIg,  228. 
86.    A.  J.  S.  XXI3,117. 
87.    A.  J.  H.  XXXIX3,  395. 
88.    A.  J.  S.  XXXII3.  304;   XXXIIIg,  115. 
89.   A.  J.  S.  XXX  VI  3.  275. 
90.    A.  J.  S.  XXVIIlg,  299  ;  XXX3,  312. 
91.   A.  J.  S.  XXXI  Us,  228. 
92.   A.  J.  S.  XXXI3,  145;  Proc.  A.  A.  A.  S.,  1885, 
246. 

93.  A.  J.  S.  XXX  I3,  460  ;  School  of  Mines  Quar- 
terly, Columbia  Coll.,  VII,  No.  2,  188. 
94.   A.  J.  S.  XXXIV3,  381. 
95.    A.  J.  S.  XXX3,  235  ;  XXXIIg,  311. 
96. 
97.   A.  J.  S.  XXXIII3,  233. 
98.   A.  J.  S.  XXXVI3,  276. 
99.   A.  J.  S.  XXXIVs,  475. 
100.   A.  J.  S.  XXXIV3.  387,  476. 
101.   A.  J.  S.  XXX  IV,,  471. 
102.  Science,  N.  Y.,  March  7,  1890,  167. 
103. 
104. 
105. 
106. 

322 


EASTMAN. 


CATALOGUE    III  -Discoverer 


Number. 

Locality. 

Iron  or  stone. 

Weight. 

1 

I. 

1     Ib. 

2 

I 

30000     11  is 

3 

Crawford  Co    Arkansas                        

S. 

14" 

4 

British  America 

I 

386       " 

5 

Canyon  City  Trinity  Co    Cal                

.   I. 

,.,        • 

6 

I. 

80      " 

7 

San  Bernardino  Co  ,  Cal  

8. 

g 

I. 

3853     Ib* 

9 

I. 

10 
11 

Sierra  de  Chaco,  Chili  

8.  A  I. 

72.75  " 

12 

Oazaca  Mexico  .        

I. 

13 

San  Luis  Potosi  Mexico 

I 

14 

Xiquipilco,  Mexico  

I. 

108  6    " 

15 

Mexico                    ..                                                      . 

I 

192      " 

16 

Mexico  

I. 

17 

Mexico 

I 

18 

I. 

2,942     Ibs 

19 

Mexico 

0.5  Ib. 

20 

Mexico  

I. 

21 

Mexico 

I. 

f>(MK>     lY.s 

22 

I. 

'III        " 

23 

Ironton   Missouri                     . 

24 

I. 

12'»      Ibs 

25 

I 

11        " 

26 

I. 

li        " 

27 

290      " 

28 

• 

14" 

29 

s 

ft  5   " 

30 

Augusta  Co   Va 

I. 

:i  r>  " 

31 

3(j      " 

32 

Augusta  Co  ,  Va              

j 

56      " 

33 

Augusta  Co.,  Va  

r 

22" 

34 

I. 

35 

Chili  

I 

9r>  5  Ib^ 

36 

I 

2  oz 

1.  A.  J.  S.  XXXIV8,  59. 

2.  A.  J.  S.  XV2,  12. 

3.  Owen's  2d  Geological  Reconnaissance  of 

Ark.,  408. 

4.  Trans.  Roy.  Soc.  Canada,  IV,  sect.  Ill,  97. 

5.  A.  J.  8.,  XXIX8,  469. 

6.  A.  J.  S.  IV3,  495. 

7.  A.  J.  8.  XXXV3,  490. 

„      f  A.  J.S.  X1X2,  163;  II8,  335;  III3,  207. 

'    I  Proc.  A.  A.  A.  8.  1871,  '266. 
9.  Buchner,  127. 

10.  Buchner,  131. 

11.  A.  J.  S.  XXXVIIg,  439. 

12.  A.  J.  S.  XV2,  21. 

13.  Buchner,  149. 

14.  A.  J.  S.  XVo,  20;  XXI12,374;  XXIV2,  295. 

15.  A.  J.  S.  XXIX3,  232. 

16.  Proc.  A.  A.  A.  S.  1871,269. 

17.  Proc.  A.  A.  A.  S.  1871,  269. 


PROGRESS  OF   METEORIC   ASTRONOMY   IN   AMERICA.  323 

Meteorites    without    Date. 


Number, 

Authority. 

Remarks. 

1 

2 
3 
4 
5 
6 
7 
8 
9 
10 
11 
12 
13 
14 
15 
16 
17 
18 

19 
20 
21 
22 
23 
24 
25 
26 
27 
28 
29 
30 
31 
32 
33 

34 

35 
36 

R.  B.  Riggs  

Found  in  Col.  Abort's  collection  of  minerals  presented  to  the  Na- 
tional Museum. 

Brought  to  Coburg,  Canada,  in  1869. 
Put  through  an  ore-crusher  before  its  character  was  known. 

Numerous  pieces. 

The  San  Gregorio  meteorite,  6.5  feet  long,  5.5  wide,  4.0  high. 
"The  largest  yet  found  in  that  vicinity." 
The  "Butcher"  meteorites—  six,  weighing  290,  430,  438,  550,580, 
and  654  Ibs. 
Found  in  a  collection  of  minerals  from  Mexico. 
Now  in  National  Museum,  Washington,  D.  C.    Estimated  weight, 
2,500  Ibs. 

Small  specimen. 

| 

Property  of  the  Smithsonian  Institution;  place  of  discovery  un- 
known. 
Riggs  considers  this  a  doubtful  specimen. 
Probably  found  in  Texas. 

Found  by  "cowboys"  before  that  portion  of  Kansas  was  settled; 
fragments  weighing  in  the  aggregate  more  than  1,600  Ibs.  dis- 
covered. 
Found  about  10  or  12  leagues  east  of  the  port  of  Chanaral  ;  not  yet 
described. 
Piece  of  a  mass  found  by  a  miner. 

A.  P.  Coleman  

C.  U.  Shepard. 
C.  T.  Jackson. 
G.  P  Merrill 

J.  L.  Smith. 
J.  E.  Whitfield. 

N.  T.  Lupton. 
J   L  Smith 

J.  L.  Smith  

J.  L.  Smith 

J.  L.  Smith  

W.  M.  Pierson. 
G.  C.  Brodhead. 

J.  L.  Smith. 
C  U  Shepard 

W.  P.  Blake. 
R  B  Riggs 

L.  G.  Eakins.... 

J.  W.  Mallet. 
J.  W.  Mallet. 
J.  W.  Mallet. 
G.  F.  Kunz  and  J.  W. 
Mallet. 
F.  H.  Snow  

Ward  and  Howell  
Ward  and  Howell  

Proc.  A.  A.  A.  S.  1871,  269. 
A.  J.  S.  XLV2,  77. 

Smithsonian  Report,  1873,  419. 
A.  J.  S.  X3,  401;  X 111 3,  213. 

A.  J.  S.  XV2, 11. 

A.  J.  S.  XI1I3,  213. 

A.  J.S.  XXH3, 119. 

A.  J.  S.  XXXI3,  41. 

A.  J.  S.  XXX1V3)  60. 

A.  J.  S.  XXXIX3,  59. 

A.  J.  S.  II3,  10. 

A.  J.  S.  II3, 10. 

A.  J.S.  II3, 10. 

A.  J.  S.  XXXIII3,  58. 

Science  N.  Y.,  Vol.  XV,  No.  379, 290;  No.  384, 359 


40-Bull.  Phil.  Soc.,  Wash.,  Vol.  11. 


324 


EASTMAN. 


CATALOGUE 


Ref.  number. 

DATE. 

TIMK  OF  SHOWER. 

|j 

2-j 
°§ 
1* 

H 

Whole  num- 
ber counted. 

1 

o   . 
•c.2 

M 

Radiant  point. 

No.  ofobserv's. 

Year. 

Month. 

1 

Begin- 
ning. 

End. 

1 
2 

3 
4 

5 

6 

7 
8 
9 
10 

11 
12 
13 

14 
lf> 
16 
17 
18 
18 

20 
21 
22 
23 
24 
25 

M 
27 

28 

m 

30 
31 
32 
33 
34 
35 

M 

37 
38 
39 
40 
41 
42 

«a 

44 

4.-, 
4ei 
47 
4S 
4i» 

BO 

1803 
1833 

1834 
1834 
1835 

1835 

1835 
1836 
1836 
1836 
1836 
1836 
1836 

1836 
1837 
1837 
1837 
1837 
1837 
1837 
1837 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1838 
1839 
1839 
1839 
1839 
1839 
1839 
1839 
1839 
1839 
1839 

April... 
Nov  

ii 

19 
13 

12 
12 
13 

h.      TO. 

13      0 
9      0 
14    50 

h.    TO. 
15      0 

Sunrise 
17    25 

h.    w. 

8<X) 

16      0 
17      0 

200,000 

18 
Many. 

"  Bend  of  the  Sickle  "  in  Leo 

1 

u 

13 

M 

13 

ii 

12 
12 
12 
I9 

14      0 
15      0 
15    30 

16      0 
18    15 
16      0 

15""4o" 

248 
253 
29 
23 
75 
500 

18 

1 

u 

12 



il 

1? 

• 

12 

AUR.  - 

Nov  
"t  ••• 

April... 
Aug.  ... 

«i 
Nov.  ... 

• 

Dec  
ii 

April'.'.'. 
ii 

Aug.::: 
it 

9 
12 
12 
12 
12 
12 
12 
20 
8 
9 
9 
10 
10 
10 
10 
11 
12 
13 
22 
6 
7 
7 
8 
11 
12 
15 
18 
18 
19 
19 
4 
9 
9 
10 
10 
10 

8      0 
13      5 
14      0 
14      0 
14    45 
15    15 
15    45 
10      0 
11     30 
9    30 
15      0 
8    55 
9      0 
9    30 
14    30 
12      0 
12      0 
13      0 
13    20 
8      0 
8      0 
10      0 
7    15 
8    45 
6      0 
6      0 
12      0 
.14      0 
12    15 
14      0 
9      0 
9      7 
12    41 
9      0 
9      0 
9    30 

15      0 
Sunrise 
ii 

18      0 
16    37 
17    15 
17      0 
16      0 
12    30 
16    20 
15    45 
10      0 
11      0 
16      0 
16      0 
18      0 
17      0 
17    20 
15    30 
17      0 
11      0 
11      0 
9      0 
10      0 
13    30 
9     15 
15      0 
16      0 
13     15 
16      0 
11       0 
14      7 
15    36 
16      0 

a  —  55°  6  —  -+-  00°  

1 
8 
1 
1 
11 
1 

I 

1 

1 
1 
;{ 

T 

8 
8 
6 
I 

3 
3 

1 

4 

I 
2 

4 
1 
I 

1 

16    30 
............ 

226 
70 
45 
74 
34 
52 
154 
20 
54 
24 
M 
48 
122 
65 
199 
131 
233 
50 
113 
210 
78 
59 
18 
28 
9 
58 
25 
19 
25 
36 
691 
100 
187 
76 
33 

.:::::::: 

In  Leo.... 

ii 

17 

In  Leo 



a  =55°,  8=  +  60°  
a  —  35°,  6  —  +  69°     

16    15 





In  Cassiopeit.' 

....„„. 

37 
80 
25 

Near  e  Cassioj>t\r  
"Sword  handle  of  1'er^eu-". 
In  Leo    

15    30 
13    30 
15    30 
14    30 

ii 

it 

In  Perseus  







a  —  273°,  6  —  -L-  45°      





"l3"30 

"Tg'i" 

Vicinity  of  ('assiopen-  
Sword  handle  of  Perse  u>  

6<; 

10      0 

"Algenib"  

1.  A.  J.  S.  XXX  VIi,  358;    Va.  Gazette  and 

12.   A.  J.  S.  XXXl!,  391. 

General  Advertiser,  April  23,1803;  N.  H. 
Gazette,  May  31,  1803;  Med.  Repository, 

13.    A.  J.  S.  XXXllt  392. 
14.   A.  J.  S.  XXX  Hi,  392. 

N.  Y.,  Vol.  1,  1804. 
2.   A.  J.  S.  XXVx,354,  3f,3. 
3.   A.  J.  S.  XXVlIj,  335:  XXVIII,,  305. 
4.    A.  J.S.  XX  Vila,  339. 
5.   A.  J.  S.  XXX!,  375. 

7.'  A.  J.  S.  XXXi,376. 
8.   A.  J.  S.  XXXIi,  390. 
9.   A.  J.  S.  XXXlj,  388. 
10.   A.  J.  S.  XXXIi,  390. 
11.   A.  J.S.  XXXIi,  389. 

15.   A.  J.  S.  XXXIlIj,  133. 
16.   A.  J.S.  XXXIIIi,37!t. 
17. 
18.        " 
19. 
20. 

22!    A.  J.  S.  XXX  I  V,,  393. 
23.   A.  J.  S.  XXXV,,  li'.T. 
24.         " 

PROGRESS  OF   METEORIC   ASTRONOMY    IN    AMERICA.  325 

IVleteor     Showers. 


5 

= 

3 
C 

1 
1 

2 

3 

4 
5 

6 

7 
8 
9 
10 
11 
12 
13 

14 

15 
16 
17 

18 
19 

20 

a 

22 
23 
24 
2.5 
26 
27 
-- 
29 
30 
31 
32 
38 
34 
35 
36 
37 
38 
39 
40 
41 
42 
43 
44 
45 
46 
47 
48 
49 
50 

Authority. 

Place  of  observation. 

Remarks. 

Richmond,  Va.,  and  Ports- 
mouth, N.  H. 
New  Haven,  Conn  

Philadelphia,  Pa. 

u  Fell  too  fast  to  be  counted." 

Number  estimated;  seen  throughout 
the  Atlantic  and  Gulf  States. 

Observed  on  the  morning  of  the  13th. 
"Unusual  number;"  hourly  rate  es- 
timated at  40  or  50. 
"  Unusual  number."   Observed  on  the 
morning  of  the  14th. 
"Unusual  number." 
Many  seen  that  were  not  recorded. 

Cloudy. 
Observed  one  hour. 
Whole  number  estimated  at  400. 

Counted  between  200  and  300. 
Majority  left  trains. 
Many  trains. 

Only  two  observers  after  17  hours. 

Prof.  D.  Olmstead  • 

Prof.  A.  D.  Baehe.,  
Prof.  A.  C.  Twining..... 

Amenia,  N.  Y  
1ft  St  Mary's  College,  Md.. 

Salisbury,  N.  C_  _  
New  York,  N.  I  
Spring  vale,  Me. 
New  Haven,  Conn  
Cambridge,  Mass  
Newark,  N.  J  

S.  Dunster  



Randolph  and  Macon  Col- 
lege, Va. 
Hingham,  Mass. 
\ew  York,  N.  Y  

J.  L.  Russell  
G  C  Schaeffer 

Prof.  D.  Olmstead  
G.C.Sehaeffer  
Prof.  F.  A.  P.  Barnard. 

New  Haven,  Conn  
New  York,  N.  Y  
New  York,  N.  Y. 
Hudson,  Ohio. 
New  Haven,  Conn. 
ML  rfL  Mary's  College,  Md. 
Knoxville,Tenn. 
Barren  Hill,  Pa. 
Wilmington  Island,  Ga. 
Society  Hill,  S.  C. 
Norfolk,  Va. 
New  Haven,  Conn. 
Wilmington  Island,  Ga. 
Rock  Island,  III. 
Cambridge,  Mass  
Cambridge,  Mass. 
Cambridge,  Mass. 
Cambridge,  Mass. 
New  Haven,  Conn. 
New  Haven,  Conn. 
Middletown,  Conn. 
New  Haven,  Conn. 
New  Haven,  Conn. 
New  Haven,  Conn. 
New  Haven,  Conn. 
New  Haven,  Conn. 
Hudson,  Ohio. 
New  Haven,  Conn. 
Hudson,  Ohio. 
New  Haven,  Conn. 
New  Haven,  Conn. 
Columbia,  Tonn. 
Middletown,  Conn. 
New  York,  X.  Y. 
Middletown.  Conn. 

E    Fitch 

L.  Obermeyer  
Prof  Wright 

ft.  C.  Sehaeffer  
T  R  Dutton           

W.  A.  Sparks  
J   D   Dana     

E.  C.  Herrick  
T   R  Dutton 

C.  G.  Forshey  
Prof.  J.  Lovering-  
Prof.  J.  Lovering  
Prof.  J.  Lovering  
Prof.  J.  Lovering  
F  C   Herrick 

F  <'   Herrick     

Prof.  A.  W.  Smith  
B.C.  Herrick  
;  E.  C.  Herrick  
E.  C.  Herrick  
E.  C.  Herrick  
B.C.  Herrick  
Prof.  E.  Loomis  
E.  C.  Herrick  
Prof.  E.  Loomi?  
E.  C.  Herrick  
E  C.  Herrick  

T.  R.  Dutton  
L.  L.  Knox  
Charles  Baldwin  
Prof.  A.  W.  Smith  

25.  A.  J.  S.  XXXV,,  167. 

26.  "  "  " 


29'.  Trans.  Am.  Phil.  Soc.  VII,  266. 
30.  A.  J.  S.  XXXV,,  323. 


34'.  A.  J.  S.  XXXV!,  361  ;  XXXVI,,  355. 

35.  A.  J.  S.  XXXV,,  361. 

36.  "  "  " 

37.  «  «  « 


38.  A.  J.  S.  XXXV,,  361. 
39. 

4L  A.  J.  S.  XXXVI,,  Ml. 

42. 

43.        ^  ^ 

tt  A.  J.  S.  XXXVII,.  325. 

46.  A.  J.  8.  XXXVII,.  325. 

47.  A.  J.  8.  XXX  :VIII,  ,203. 

48.  A.  J.  S.  XXX\  I.,,  325. 

»• 

50.        " 


326 


EASTMAN. 


Ref.  number,  j 

DATK. 

TIME  or  SHOWER. 

Time  of  max. 
flight. 

Whole  num- 
ber counted. 

£> 

'— 

h 

.2 

S 

Radiant  point. 

f 

I 

•5 

0 

SS 
4 

3 
:; 
l 
4 
1 
1 
1 
3 
1 

1 

5 

7 
7 
7 
•J 
4 
1 
4 
•J 
1 
4 
2 
1 
4 
4 
» 
3 

:; 

4 

3 

.; 

3 
3 
8 

1 
1 
1 
3 
1 
1 
1 
1 
1 
1 
1 
3 
4 
1 
7 

Year. 

Month. 

1 

10 
10 

11 

14 
9 
9 
9 
10 
18 
19 
9 

10 
20 
8 
9 
10 
13 
9 
10 
11 
12 
9 
10 
11 
10 
10 
11 
9 
9 
9 
19 
10 
9 
10 
10 
9 
10 
9 
10 
11 
11 
12 
10 
9 
9 
10 
10 
11 
29 
5 
9 
9 
9 
9 

Begin- 
ning. 

End. 

51 
52 
53 
54 
55 
M 
57 
H 
H 

ao 

01 
62 

u 

f.4 
85 

66 
87 
8H 

CO 
70 
71 
72 
7.", 
74 
75 
78 
77 
7S 
70 

80 
81 
s-j 
K:< 
M 
8fi 
88 
81 
88 
8U 

!»0 
111 
!»2 
:i:5 

M 

95 
06 

!'7 

'.(S 

N 

100 
101 
102 
103 
104 

1839 
1839 
1839 
1839 
1840 
1840 
1840 
1840 
1841 
1841 
1841 

1841 
1842 
1842 
1842 
1842 
1842 
1844 
1844 
1844 
1844 
1845 
1846 
1846 
1847 
1847 
1847 
1848 
1M8 
1848 
1849 
1849 
1850 
1850 
1850 
1852 
1853 
1855 
1856 
18,55 
1855 
1855 
1856 
1858 
1858 
1858 
1858 
1858 
1859 
1859 
1859 
1859 
1859 
1860 

Aug.... 
ci 

April'.!'. 
Aug.  ... 

M 

April'.!'. 
Aug.  ... 

N<w..!!! 
Aug.... 

U 
|| 

April'.!! 
Aug.... 

"  '.!! 

Ci 

•1 

H 

July!! 
Aug.  .. 

ti 
ii 

h.    m. 
10      0 
11    20 
9      0 
10      0 
8      0 
10       0 
14     15 
15      0 
8    30 
11      0 
12      0 

9      0 
10    20 
9    50 
10      0 
10    10 
15      0 
11     20 
8      0 
9    50 
13    50 
10      0 
12      0 
9      0 
10      0 
12      0 
9     15 
13      0 
13    30 
15      0 
13      0 
10      0 
12    40 
10      0 
12      0 
14      0 
11    45 
10    25 
10    30 
10      0 
13    55 
13    30 
11      5 
10    45 
12      5 
8    30 
13      7 
14    15 
10    30 
11      0 
11      0 
13      0 
14    15 
10      0 

h.    m. 
13      <) 
12    20 
10      0 
12      0 
16      0 
15    30 
15    45 
15    35 
11    30 
13      0 
15      0 

10      0 
16      0 
16      0 
12      0 
11       0 
16      0 
15      0 
13      0 
15      0 
15      0 
13      0 
14      0 
10       0 
12       0 
14      0 
10      0 
15    30 
15    30 
16    45 
14      0 
12    30 
15      0 
12      0 
15      0 
14    40 
15    25 
14    30 
13      0 
11      0 
16      5 
14    45 
14    50 
15    10 
14      5 
9      0 
13    52 
15    15 
11     30 
12      0 
13      0 
15    30 
15    30 
15    10 

h.    m. 
13     0 

491 
50 
28 
72 
171 
818 
112 
88 
60 
20 
49 

60 
151 
90 
133 
89 
46 
367 
117 
622 
46 
81 
46 
41 
41 
415 
37 
476 
216 
55 
64 
260 
451 
312 
351 
19 
408 
385 
90 
37 
58 
36 
283 
128 
56 
11 
29 
33 
16 
19 
64 
304 
56 
588 

189 

Sword  handle  of  Perseus  
i>                     it 

Bet.  Cassiopese  and  Perseus.. 
Sword  handle  of  Perseus  

a  _  30o  5  —  -}.  530  30- 

............ 

44 

"332" 
76 





a  =  198°,  «  =  -8°  

"iJTso" 

""Ks" 
......... 

Corona  Boreali*  

Sword  handle  of  Perseus  

"isT'sb" 

139 
"TsT 

/3  Cassiopese  

14      0 

!"!!!!!! 

Sword  handle  of  Perseus  



Head  of  Perseus 

15    15 

281 

In  Perseus  

In  Perseus  

13    30 

216 

In  Perseus 

"iT'sb" 

13    30 
13    30 

"is?"  so" 

14    35 

119 
110 
136 

"Too" 

Sword  handle  of  Perseus  
ii                     tt 

ii                     tt 



15    15 

156 

"TM" 

Sword  handle  of  Perseus  
a  =  38°  30',  6  =  -4-  57°  15'  
Sword  handle  of  Perseus  

14    30 

51.   A.  J.S.  XXXVI  Ilt  325. 
52.  Trans.  Am.  Phil.  Soc.  VII, 
53.             " 
54.   A.  J.S.  XXX  VI  IL  325. 
55.  Trans.  Am.  Phil.  Soc.  VII. 
56.  A.  J.  S.  XXXIXj,  328. 
67. 
68.        "               "             " 
59.  A.  J.  S.  XLII,,  397. 
60. 
61.  A.  J.  S.  XLL.  390. 
62.        "             "         " 
63.   A.  J.  S.  XLIIIi.  212. 
64.  A.  J.  S.  XLIIIi,  377. 

268. 
270. 

65.  A.  J.  S.  XLIIIj,  377. 

66.  "  "  " 

67.  A.  J.  S.  XLIV,,  209. 

68.  A.  J.6.  XLVIIIj.316. 

69.  A.  J.  S.  XLVIII,,320. 

70.  A.  J.  S.  XLVIIIJ.31G. 

71.  " 

72.  A.  J.S.  L>,  86. 

73.  A.  J.S.  HIo,  125. 

74.  "  ••       »' 

75.  Sidereal  Messenger,  II,  14. 

76.  A.  J.  S.  VIo,  278. 

77.  "          ""    " 

78.  A.  J.  S.  VI2,  279. 


PROGRESS   OF   METEORIC   ASTRONOMY   IN    AMERICA. 
Meteor    Showers— Corat'cl. 


327 


Ref.  number. 

Authority. 

Place  of  observation. 

Remarks. 

51 

E  C  Herrick  

New  Haven,  Conn. 

52 

C  G   Forshey 

St  Loui?,  Mo. 

53 
54 

C.  G.  Forshey  

E  C  Herrick        .    .. 

Illinois  River. 
New  Haven,  Conn. 

55 

C.  G.  Forshey  

Philadelphia.  Pa. 

56 

E  C  Herrick 

Moon  set  at  14h  Om 

57 

G  C  Schaeffer 

Jamaica  L.  I 

58 

G  C  Schaeffer  

Jamaica,  L.  I. 

59 

C  G  Forshey 

Vidalia   La     

No  trains  ;  paths  short. 

60 
61 

62 

E.G.  Herrick  
Dr.  J.  S.  Huntington, 
U.  S.  N. 
Dr  John  Locke  

New  Haven,  Conn. 
Pensacola,  Fla. 

Cincinnati,  Ohio. 

63 

E  C  Herrick 

New  Haven   Conn       

Moon  set  at  I5h.  Om. 

64 

E  C  Herrick 

Cloudy  •  actual  observing  time  Ih  10m 

65 

E  C  Herrick 

New  Haven  Conn  

Cloudy. 

66 

E  C  Herrick  

New  Haven,  Conn  

Cloudy, 

67 

E  C  Herrick 

New  Haven  Conn  

Cloudy  after  16h. 

68 

E  C  Herrick 

Partially  cloudy. 

69 
70 

S.  R.  Williams  
E  C  Herrick  

Canonsburg,  Pa. 
New  Haven,  Conn. 

71 

E  C  Herrick         .   .  .. 

New  Haven  Conn. 

72 
73 

E.C.  Herrick  
E  C  Herrick        

New  Haven,  Conn  
New  Haven,  Conn. 

Cloudy. 

74 

E  G  Herrick 

New  Haven  Conn 

75 

C  G   Forshey      

33  conformable  with  the  radiant. 

76 

W   M  Smith 

Manlius  N  Y  

Cloudy  after  14h. 

77 

E  C  Herrick 

Completely  cloudy  after  lOh. 

78 

E  C  Herrick 

New  Haven  Conn. 

79 

E  C  Herrick  

"On  Mt.  Carmel." 

80 

C  G  Forshey  

Mouth  of  Miss,  river. 

81 
82 
83 

E.  C.  Herrick  
S.  R.  Williams  
E  C  Herrick 

New  Haven,  Conn. 
Canonsburg,  Pa. 
New  Haven  Conn. 

• 

81 

E  C  Herrick  

New  Haven,  Conn. 

85 

E  C  Herrick 

New  Haven   Conn. 

86 

John  Edmunds  

New  Haven,  Conn. 

87 

E  C  Herrick 

New  Haven  Conn. 

88 

E  C  Herrick 

New  Haven   Conn  

306  conformable. 

F  C  Herrick 

242  conformable. 

90 
91 

E.C.  Herrick  
E  C  Herrick 

New  Haven,  Conn  

One-half  conformable. 
45  conformable. 

92 

E.  C.  Herrick  

New  Haven,  Conn  

20  conformable. 

93 

E  C  Herrick  

New  Haven,  Conn. 

94 

Observed  on  railroad  between  Daven- 

95 
96 
97 
98 

Prof.  A.  C.  Twining  ... 
Prof.  A.  C.  Twining... 
Prof.  A.  C.  Twining  ... 
Prof.  A.  C.  Twining  ... 
F   Bradley 

Cleveland,  Ohio. 
Cleveland,  Ohio. 
Cleveland,  Ohio. 
Cleveland,  Ohio. 
Chicago  111 

port  and  Chicago,  111. 
6  conformable  to  the  August  radiant. 

100 

F  Bradley 

8  conformable  to  the  August  radiant. 

101 

F  Bradley 

Chicago,  111. 

10° 

F  Bradley 

Chicago  111     

Only  a  few  unconformable  meteors. 

103 
104 

Prof.  A.  C.  Twining  ... 
E.C  Herrick  

Boston,  Mass. 
New  Haven,  Conn. 

J.  S.  VIo,  279. 
J.  8.X  U,  133. 
J.  S.  VI  llj,  429. 


J.  S.  XIVo,  430. 
J.  S.  XVIs,  288. 
J.  S.  XX2,  285. 


79.  A. 

80.  A. 

81.  A. 
82. 

83.  A.  J.  S.  XI2,  130. 

84.  "  "        u 
85. 

86.  A. 

87.  A. 

88.  A. 
89. 
90. 

91.  A.  J.  S.  XX2,  285. 


A.  J.  S.  XX2,  285. 
*.  XXII, 


A.  J.  8.  XXII2,  290. 

94.   A.  J.  S.  XXVJo,  435. 

95. 

96. 

97. 

98. 

99.   A.  J.  S.  XXVIIIo,  446. 
100.        " 
101. 
102. 
103. 
104.  A.  J.  S.  XXX2,  296. 


328 


EASTMAN. 


IV.- 


Ref.  number. 

DATE. 

TIME  or  SHOWER. 

Time  of  max. 
flight. 

Wrhole  num- 
ber counted. 

jj 

1 

Radiant  point. 

No.ofobserv's. 

Year. 

Month. 

i 

Begin- 
ning. 

End. 

105 
106 

107 
108 

109 

110 
111 

113 

114 
115 
116 
117 
118 
119 
120 
121 
122 
123 
124 
125 
126 
127 
128 
129 
130 

132 
133 
134 

137 
138 

M"'i 
141 
142 
143 
144 
145 
146 
147 
148 
149 
150 
151 
152 

153 
154 

155 

1860 

1863 
1863 

1863 

Aug.  ... 

NOV.  ::: 

(t 

M 

Dec.  ... 

April... 
July  ... 
Aug.  ... 

ti 

NOV.  ::: 

Aug.::: 
NOV..::: 

H 

Aug.  ... 
u 

NOV..::: 

9 
10 
7 
12 

12 

13 
13 
14 
12 

19 
3 
10 
10 
10 
10 
10 
11 
11 
10 
11 
11 
11 
12 
12 
12 
12 
13 
13 
13 
9 
10 
13 
13 
18 
10 
in 
in 

10 

10 
10 
10 
10 

11 
11 
11 

12 
12 
13 

13 
13 

13 

h.   m. 
11    30 
11      0 
7      0 
6    30 

10      0 

6    15 
15    15 
15    40 
8    20 

14    45 
9      5 
8      0 
10      0 
10    25 
10    30 
12    25 
8     15 
9    30 
13      0 
14    15 
14     15 
16      0 
15      0 
15      0 
11     15 
15    20 
10      0 
15      0 
15     15 
•14      0 
12    30 
12      0 
15    15 
Hi     30 
8    30 
9      II 
9      0 
9     15 
10      0 
12       0 
13      0 
15     10 
9      0 
10      0 
11     22 
10      0 
10    20 
8      0 

9    30 
10     10 

10    38 

h.   m. 
13     o 
14     0 
9      0 
17      0 

16      0 

17      0 
16    15 
16    25 
12      0 

16      0 
10      5 
15    15 
13      0 
14    45 
.13      0 
13      0 
10    15 
12      0 
15      0 
16    40 
15    30 
17      0 
17      0 
16    30 
12     15 
16    20 
.13      0 
17     3H 
17    38 
15    40 
15    30 
15      0 
17      5 
17    30 
10      0 
12      0 
13      0 
10     15 
13    50 
14      0 
14      0 
15    40 
11      0 
15      0 
14    52 
14      0 
15    51 
14      0 

13    30 

17      7 

17    16 

h.   m. 

57 
381 
46 
423 

381 

500 
•21 
15 
180 

52 
36 
397 
289 
289 
95 
MO 
62 
47 
11 
:;j 

15 
130 
15 

'"146" 

Sword  handle  of  Perseus  
a      32°  6      -f-  61° 

1 
5 
8 

12     30 
"14"  "36" 
14    30 
13    30 

N.  E.  of  zenith  

68 
90 
83 
......... 

In  Leo 

5 

In  the  "Sickle"  in  Leo.... 

K                          It                      II 

1 
1 

........... 

4 

2 
4 

8 

I 
I 
2 
1 
2 
1 
1 
1 
4 
2 
8 
1 
3 
1 
6 
1 

12    30 
12    30 

"12"  "30" 

75 
119 
85 

ft  Peisfi 

Hword  handle  of  Perseus  
Between  T/,  y,  and  T  Pers»-i  ... 
In  Perseu.s         

37 

....„„. 

In  IVr>eus 

a  =  166°  30',  &=  +40°  40'  
Near  y  Leoni« 

In  Leo  

u 

:::::::::::: 

11 

27 

u 

19 

90 
51 
59 
31 
17 
41 



Zenith  



In  Perseus  .           



:::::::::::: 

In  Leo.... 

M 

1  ii  1  Vr^ciis.         

'.Hi 

130 
289 
87 
153 
67 
105 
185 
129 
199 
107 

32 
213 

316 









8 

15    30 

46 
69 

In  Leo  

6 

7 

In  the  "Sickle"  in  Leo  

105.   A.  J.  S.  XXXIo,  136. 
106. 
107.  A.  J.  S.  XXXIn,  137. 
108.  A.  J.  S.  XXX  I2,  138. 
109    A  J  S.  XXX  I2  139 

118.   A.  J.8.  XXXII.,,  294. 
119.   A.  J.  S.  XXXIlT,,  447. 
120.  A.  J.  S.  XXXII,,  295. 
121.   A.  J.  S.  XXXIllo,  148. 
122.   A.  J.  S.  XXXIIo,  447. 

110.  A.  J.  S.  XXXL,  138. 
111.   A.  J.  S.  XXXf2,  137. 
112.        "              " 
113.   A.  J.  S.  XXXIo,  138. 
114.   A.  J.  S.XXXII2,  294. 
115.   A.  J.  S.  XXXII2,29G. 
116.   A.  J.  S.  XXXII2>  294. 
117. 

123.   A.  J.  S.  XXXIIi.,,  148. 
124. 
125.  A.  J.  S.  XXXIII2,  146. 
126.        "                "        '      " 
127.         " 
128.   A.  J.  S.  XXXIII,,  147. 
129.   A.  J.  S.  XXXIII,.  148. 
130. 

PROGRESS  OP   METEORIC   ASTRONOMY   IN   AMERICA.  329 

Showers—  Cont'd.. 


Ref.  number. 

Authority. 

Place  of  observation. 

Remarks. 

105 

F.  Bradley  

Chicago,  111. 

lor. 

F.  Bradley 

Chicago    III. 

107 
108 

Prof.  C.  U.  Shepard  
Francis  Miller 

Off  Cape  Hatteras. 
Montgomery  Co.  Md  

ob- 

109 

Prof.  D.  Kirkwood 

Bloomington,  Ind  

servations. 

ftor 

110 

Francis  Miller  

Montgomery  Co.,  Md  

13h. 

ob- 

111 

112 
113 

114 

Prof.  H.A.Newton  
Prof.  H.  A.  Newton  
Francis  Miller  

E.  C.  Herrick 

New  Haven,  Conn. 
New  Haven,  Conn. 
Montgomery  Co.,  Md  

New  Haven,  Conn  

servations. 

Several  students  assisted   in  the 
servations. 

ob- 

115 

E.  C.  Herrick  

New  Haven,  Conn. 

110 

F.  W.  Russell 

Natick,  Mass. 

117 

E  C  Herrick 

New  Haven   Conn 

118 

B.  V.  Marsh  

Burlington,  N.  J  

A  very  large  meteor  at  llh  23m. 

119 
V>0 

Prof.  A.  C.  Twining  ... 
R.  M.  Gummere  

New  Haven,  Conn. 
Burlington,  N.  J. 

1^1 

John  Roberts  

Madison,  Ind. 

1-22 
1"3 

Prof.  A.  C.  Twining  ... 
F.  W.  Russell 

New  Haven,  Conn. 
Natick   Ma«s. 

1?4 

F.  W.  Russell  

Natick,  Mass. 

125 

1?6 

Prof.  A.  C.  Twining  ... 
E.G.  Herrick  

New  Haven,  Conn. 
New  Haven,  Conn. 

1*7 

l'/8 

Prof.  A.  C.  Twining  ... 
S.  J.  Gum  mere  

New  Haven,  Conn. 
Burlington,  N.  J. 

129 
130 

131 

Prof.  D.  Kirkwood  
Prof.  D.  Kirkwood  
F.  W.  Russell  

Bloomington,  Ind. 
Bloomington,  Ind. 
Natick,  Mass. 

132 
133 

S.  J.  Gummere  .... 
B  V  Marsh 

Burlington,  N.  J. 
Germantown  Pa         

Thirteen  left  trains. 

134 

F.  W.  Russell 

Winchendon,  Mass. 

135 

B.  V.  Marsh  

Germantown,  Pa. 

136 
137 

Prof.  S.  J.  Gummere... 
B  V  Marsh 

Haverford  College,  Pa. 
Germantown,  Pa 

138 
139 

Prof.  A.  C.  Twining  
W  G.  Bryant 

New  Haven,  Conn. 
Winchendon,  Mass. 

140 

F.  W.  Russell  .... 

Natick,  Mass. 

141 
142 
143 

J.  G.  Pinkham  1... 
Prof.  H.  A.  Newton  
B.  V  Marsh 

Manchester,  Me. 
New  Haven,  Conn. 
Philadelphia,  Pa. 

144 

F.  W.  Russell  

Natick,  Mass. 

145 

F.  Bradley  

Chicago,  111. 

146 
147 

Prof  H.A.Newton  
F.  W.  Russell        .      .  . 

New  Haven,  Conn. 
Natick,  Mass. 

148 
149 
150 
151 
152 

153 

Prof.  O.N.  Stoddard.. 
Prof.  H.  L.  Smith  
Prof.  O.  N.  Stoddard.  . 
Prof.  H.  L.  Smith  
Prof.  A.  D.  Bache  

Prof  H  A  Newton 

Oxford,  Ohio. 
Kenyon  College,  Ohio. 
Oxford,  Ohio. 
Kenyon  College,  Ohio. 
Coast  Survey  Office,  Wash- 
ington, D.  C. 
New  Haven   Conn  

.More  than  half  the  tracks  plotted 
Hazy. 

154 

155 

Capt.    J.    M.    Gilliss, 
U.  S.  N. 
Prof.  S.  J.  Gummere... 

U.  S.  Naval  Observatory  
Haverford  College,  Pa  

Track  of  each  meteor  plotted. 
200  tracks  plotted. 

131.  A. 

132.  A. 
133. 
134.   A. 
135. 
136.  A. 
137. 
138. 

139.  A. 

140.  A. 

141.  A. 

142.  A. 

143.  A. 


J.  S.  XXXIII2,  148. 
J.  S.  XXXIIlo,  147. 

J.  S.  XXX I V2,  295. 
J.  S.  XXXV2, 146. 


J.  S.  XXXVIo,  30G. 
J.8.  XXXV U,  305. 
J.S.  XXXVIo,  304. 
J.  8.  XXXVL,,  302. 
J.  S.  XXXVl'o,  304. 


144.  A. 
145. 

146.  A. 

147.  A. 

148.  A. 

149.  A. 

150.  A. 

151.  A. 

152.  A. 

153.  A. 

154.  A. 

155.  A. 


J.  S.  XXX VI2,  305. 

J.  S.  XXXVIo,  302. 
J.  S.  XXXVI2,305. 
J.  S.  XXXVIio,  144. 
J.  S.  XXXVIIo,  146. 
J.S.  XXXVIIo,  144. 
J.  S.  XXXVllo,  146. 
J.S.  XXXVllo,  145. 
J.  S.  XXX  VI 4  143. 
J.S.  XXXVllo,  141. 
J.S.  XXXVII2, 142. 


330 


MAN. 


CATALOG-UK    IV.— 


E 

= 
c 

• 

DATE. 

TncEorSHOWEE. 

Time  of  max. 
Bight 

Whole  num- 
ber count.  -.1. 

Max.  hourly 

I-UU'. 

Radiant  point. 

Year. 

Month. 

L 

B*gin- 
ning. 

End. 

156 

1.17 
Ml 
159 
15&! 
161) 

161 

Ml 

164 
M 
Ml 
Ml 

Ml 
Mi 

170 

171 

17  J 

in 

174 
175 

177 
17- 
179 
180 
181 
182 
183 
184 
185 
186 
187 
188 
189 
190 
Itfl 
192 
193 
194 
195 
196 
197 
198 
199 
200 
Ml 
202 
203 

MI 

205 
206 

1863 
1  M 
MM 
MM 
MM 
MM 

MM 

MM 

1864 
1864 
1864 
1864 
1864 
1864 
1864 
1865 
MM 
1865 
1865 
1865 
MM 
1866 
1866 
MM 
MM 
MM 
MM 
1866 
MM 
1866 
1866 
1866 
1866 
1866 
1866 
1866 
1866 
1866 
1866 
)-...; 
MM 
MM 
MM 
MM 
MM 
MM 
1866 
MM 
MM 
MM 

1866 

1-,-, 
1866 

NOT.  .. 

44 

44 

44 
44 

13 

13 

n 
u 

u 

9 
12 
15 

IJ 
9 
9 
10 
10 
10 
M 

10 
10 
10 

11 
11 
1 
1 

11 

12 
12 
12 
IJ 
U 
12 
12 
12 
U 
1-J 
U 
U 
IJ 
13 
13 
13 
13 
13 
13 

79 
M 
17 
33 

29 

332 

44 

25 
-  .1 
50 
18 
46 
19 

M 
178 

.     63 

114 
50 
364 
1(10 
129 
164 
51 
75 
8 
63 
93 
47 
27 
205 
85 
402 
236 
65 
603 
35 
8 
56 
458 
64 
8 

26 

In  the  "Sickle"  in  Leo  

4*                                              44 

1 

J 

13     0 
15     0 
15    45 
9      0 
10      0 
10    20 

10    30 
10    30 
10    40 
11    30 
12      0 
13      0 
15      0 
13     15 
13    45 
14    25 
10    45 
11 
13 
15 
9 
12 
9 
9    10 
9    15 
12      0 
12      0 
13      0 
14      0 
8    15 
14      0 
9    45 
10      0 
13    30 
7      0 
10    45 
11      0 
11    10 
U    30 
12      0 
13      0 
13    10 
14    20 
14    40 
15    54 
16      6 

17    20 
16    30 
17    45 
16 
11 
13 

13 
13 
12 
14    30 
U    M 
15    90 
16      0 
16    15 
16      0 
15    50 

15      5 
14      0 
16      0 

.         "n 

14      0 
10    15 
15      0 
11    30 
14    15 
14    15 
14      0 
16      0 
9      0 
16      0 

15      0 
14    30 
18      0 
14    30 
16    40 
13    40 
13      0 
17      0 
15      0 
13    40 
15    20 
17     M 
16    39 
16    36 

15  30 



44 

NOT 

"iT'sb" 

........ 
........ 

In  Leo 

NOT.  ~ 
Aug.::: 

44 
4t 

44 

44 
44 
44 

NOT.  '.L 

44 
44 
44 
44 
44 
.4 
44 
44 

44 

a  =  42°,  8 
a  —  52°,  1  y»  <f*  M 

In  the  "Sickle^'  in  Leo 
" 

12  30 

iT'ab" 

14  "so" 
13  30 
16  10 
11  30 

"is"  "so" 

i-sioppas  

1 

4 

10 
12 

5 

In  Perseus  

......... 

31 
99 
108 

"iss" 

"About  Capella"  
In  Leo_  



Between  a  and  y  Leoni*  



44 
44 

44 
44 
44 
44 

44 



"iso" 

a  =  147°30',  5  =  -23°  15'  

354 
453 
440 
Ml 

492 
901 
261 

7      0 
8    30 
10      0 
11      0 
11      0 
11    20 

18      0 
16    30 
15      0 
14      0 
16    10 
14    40 

13  30 
15  0 

71 
138 

13  0 
15  30 
12  30 

•JlJ 
113 

In  Leo                              .    ... 

156.  A.  J.S.  XXXVII,,  142. 
157.    A.  J.S.  XXX  Vlj;,  143. 
158. 
159.   A.  J.S.  XXX  VI  1  12,  432 
159!. 
160. 
161. 

IS:    •        ;;       ;; 
164!*  • 

165. 
106. 
167.  A.  J.S.  XXX  IX.,  229. 

168.   A.  J.S.  XXXIX  . 
169.   A.  J.  S.  XLs,  284. 
170. 
171. 
172.   A.  J.S.  XLK  273. 
173. 
174.   A.  J.  S.  XLIU,  280. 
175.   A.  J.S.  XLI: 
176.   A.  J.S.  XLIU,  2»r,. 
177.   A.  J.  S.  XLIIs,429. 
178. 
179.        " 
180.        " 
181.   A.J.  S.  XLIIo,  429. 

PROGRESS  OF   METEORIC  ASTRONOMY   IN   AMERICA.  331 

Showers— Cont'd. 


Authority. 


Place  of  observation. 


Remarks. 


1S6     B.  V.  Marsh.  

f«On  Nov.  13,  55  tracks  were 
Germantown,  Pa.  S  Ha*y.       plotted  in  Phila.  by  H.  D. 

1ST  1  c.  E.  Dutton  -..  

Norfol  k.  Va.                                               Vail.  56  tracks  were  oloWed 

160 
161 

J.  H.  Worrall  
H  P  Tattle 

West  Chester,  Pa-  .  

Off  Charleston,  8.  C. 
Riverside,  Kan. 
Belvidere,  N.  J. 

Chicago,  HI  — 

Ha«y.  •{     in  West  Chester  by  B.  Hoop- 
er, 27  tracks  were  plotted  in 
Easton   by  E.  Menline.   23 
tracks  were  plotted  in   St. 
Louis  by  Prot  W.  Chanvenet. 
Cloudy  in  the  Middle  and  N.  E.  States. 

G.  Scarborough...  
H.  8.  Osborn  

Francis  Bradley  — 

162     w.  H.  R.  Lykins_  !  Lawrence,  Kan. 
163  i  B.  V.  Marsh  ,  —  Philadelphia,  Pa. 
163!    Prot  H.  A.  Newton-...   New  Haven.  Conn. 

164 
165 

G.  Scarborough  _    Riverside,  Kan. 
Francis  Bradley  Chicago,  Dl. 

166 

G.  Scarborough...  •  Riverside,  Kan. 

167 

R.  H.  Stretch  Virginia  City,  Nevada. 

168 
169 

R.  H.  Stretch  •  Virginia  City,  Nevada. 
Prot  A.  C.  Twining  —  :  Hinsdale,  Mass. 

170 

Prof.  A.  C.  Twining  .  Hinsdale.  Mara. 

171 

Prot  H.  A.  Newton  \  New  Haven,  Conn. 

m 

0.  B.  Wheeler  Detroit.  Mich. 

- 

O.  B.  Wheeler 

Detroit.  Iffioh. 

174 

-' 

D.  Trowbridge  HecWVN.Y. 
Prof.  H.  A.  Newton-..-'  Sherbnrne,  N.  Y. 

176 

D.  Trowhrifim                        TT<*»tnr    V    V                                          Rnm*  loft  tr*ino  U«tin<r  Knr  7MMuui* 

177     F.  W.RusseTl  Natfek,'  MasV! 

178   1    TOMJ.  PierSOn.                       *   Vimm»*vt  Onnn<i                                  "  rMT  If  .rth.'a  VinAw.v.1     ftf  .<x> 

179     R  V.  Marsh  

Germantown,  Pa. 

MO     R.  M.  Gummere.  
181     Prot  H.  A.  Newton  

Germantown,  Pa. 
Sherbnrne,  N.  Y. 

182  1  3.  fl.  Worrall  

West  Chester,  Pa. 

183 

m 

I.  rrowbridn  
J.  H,  Worrall  
James  Ferguson  
James  Ferguson  

Hector,  N.  Y. 
We»t  Chester,  Pa. 
U.  8.  Naval  Observatory. 
U.  a  Naval  Observatory. 

1*7     F.Bradley  Chicago,  HI. 

188     Prof.  Hopkins  Williamstown,  Mass  Williams  College. 
MB     C.  G.  Rock  wood  f  Newark.  N.  J.                            No  observations    from    12h.  45m.  to 

191 

James  Ferguson  U.  8.  Naval  Observatory. 
Prot  H.  A.  Newton  I  New  Haven,  Conn. 

13h.0m. 

m 

193 
194" 

F.  Bradley  1  Chicago,  HI  ..  
C.  S.  Lyman  ~~.  New  Haven,  Conn. 
Prot  Hinriehs.....       .    Iowa  City,  Iowa. 

F.  W.  Russell,  of  Cambridge,  Mass., 
observed  several  evenings  in  first 
half  of  November,  and  counted,  in 

195     B.  V.  Marsh  Germantown,  Pa. 

all,  875  meteors. 

1§6  j  O.  B.  Wheeler.  :  Detroit.  Mich. 

197  :  Prot  H.  A.  Newton  i  New  Haven.  Conn. 

198     Prot  D.  Kirk  wood  

Canonsbnrg,  Pa. 

199  •  B.  V.  Marsh. 

Germantown.  Pa. 

300     Maria  Mitchell.  ...11-1  Vassar  College.  N.  Y  

Observed  seven  hours. 

m 

202 
303 

Prof.  Hopkins 
ProtHbuicfca  
John  T.  Wheeler  

Williamstown.  Mass  
Iowa  City,  Iowa. 
Concord,  N.  H. 

Williams  College. 

204     Prot  C.  S.  Lyman  

New  Haven,  Conn. 

305     Prot  H.  A.  Newton  

New  Haven,  Conn. 

306     C.  G.  Rockwood  

Newark,  N.J. 

IfflL  A.J.  S.  XLIIS,429. 

183.  A.  J.  S.  XLIU.286. 

184.  A.  J.  S.  XLIIj,  429. 

L  J.  S.  XLI1I,,  78;  Nov.  Meteors,  1866, 
D.  S.  N.  Obs'y,  8vo. 

186.  -  m"  m 

187.  A.  J.  8.  XLIII,,  78. 

189.  "  » 

190.  A.  J.  S.  XLIII,.  78,  Nov.  Meteors,  1866, 

U.  S.  N.  Obs'y,  8vo. 

191.  A.  J.  S.  XLIII*  78. 

192.  "  ••          • 

193.  t*  mm 

41-Bull.  Phil.  Soc.,  Wash.,  Vol.  1L 


194,  A.  J.  S-XLIUfcTU. 

195. 

196. 

197. 

198. 

199. 


thsonian  Arc  ives  (not  yet  printed). 


_  :. 
:.  ''.  h 

304.  A.    .8.  XL  II*  7*. 

•ft 

^^•A.  J.  a  XXXVII,,14L 


332 


EASTMAN. 


CA.T-A.-L.OG  U  E    IV.- 


Ref.  number.  1 

DATE. 

fine  or  SHOWER. 

Time  of  max. 
flight. 

Whole  num- 
ber counted 

j>> 

!! 
1. 

Radiant  point, 

•o 
I 

Year. 

Month. 

1 

Begin- 
ning. 

End. 

207 
208 
209 
210 
211 
212 
213 
214 
215 
216 
217 
218 
219 
220 
221 
222 
223 
224 
225 
226 
227 
228 
229 
2W 
231 
232 
333 
234 
235 
236 
237 

238 
239 
240 
241 
242 
243 
244 
245 
24h 
247 
248 
249 
250 
251 
252 
253 
254 
255 
256 
257 
258 
259 

1866 
1866 
1866 
1866 
1866 
1866 
1866 
1866 
1866 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 

1867 
1867 
1867 
1867 
1867 
1867 
1867 
1867 
1868 
1868 
1868 
1868 
1868 
1868 
1868 
1868 
1868 
1868 
1868 
1868 
1868 
1868 

Nov 

13 
13 
13 
13 
13 
13 
13 

h.     m. 
12     0 
12      0 
12      0 
14      0 
14      0 
15      8 

h.    m. 
12    36 
13      0 
17    15 
16      0 
16    30 
16      8 

h.     m. 

28 
35 

101 
180 

'S 
«8 

75 
20 
17 
35 
27 
39 
44 



1 

a  =  147°  30',  S  =-  +  24°  30'  1 

14    30 

61 

3 

14    30 

91 

a  I,  t-t  mis       4 

Bend  of  the  Sickle                      1 

6 

u 

May 

16 
17 

21  > 

13      0 
14      0 

15      0 
17    30 



Between  ^  and  e  Leonis  1 
Near  a  Leonis  1 



A  little  southeast  of  Lvru  1 
In  Perseus  1 
"             i 

Aug.  ... 

•< 
•« 
Nov.  '.'.'. 

It 
It 
II 

II 
II 
II 

8 
9 
9 
9 
10 
10 
11 
13 
13 
13 
13 
13 
18 
13 

18 
18 
18 

13 
18 
13 
18 

18 
18 

13 
13 
13 
13 
13 

!    11 

12    15 
13      3 
13      3 
14    15 
14      0 
15      0 
14      0 
9      0 
9     28 
10      0 
11       0 
11     45 
12      0 
12      0 
12     30 
13      0 
13      0 
13      0 
13      0 
14      0 
15      3 

15    45 
15    55 
16      0 
16      5 
16    30 
17      0 
17      0 

12    55 
14    30 
14    30 
15    25 
15    40 
15     30 
15    30 
17      0 
13      0 
16      0 
16      0 
18     25 
16    40 
17    45 
17      0 
18      0 
l:',    311 
16     2§ 
18      0 
18     13 
17    45 

16    45 

ir.    :r. 
17      0 
17    54 
17     30 
17     22 
17     30 

»«                    i 

"iiTSr 

17 
45 
535 
50 
4,937 
1.000 
2,325 
2,056 
3,730 
1,713 
3,044 
500 
1,474 
2,267 
1,626 
1,800 

1,088 
339 
500 
1,301 
460 
100 
61 
500 
56 
1,330 
2,886 
2,500 
1,462 
700 
5,573 
5,000 
8<K) 
5,670 
896 
850 
1,341 
1,926 

'"276" 

"             i 

"                                               1 

r 

15    30 
15    45 

1.-,    60 
i:.     -<•> 
16    30 

"I'JT'M" 

,  16    10 
16    30 

1,488 

\ 

2,184 
1,076 
2,110 

a  =  147°  45',  5=  +  2:'.  '  o'  2 

2,220 
1,472 
1,082 

4 

1 

In  Leo  1 

a  =  150°  45',  «  =  +  21°  55'  1 
a  =  148°  0',  fi  =  +  23°  0'  
•> 



:::::::::::: 



In  Leo                                           4 

1 



In  Leo           .                                1 

1 



...                              1 

Aug.  ...    o 

Nov....   13 
"     ...    13 
"     ...    13 
"     ...    13 
"     ...    13 
••     ...    13 
"     ...    13 
"      ...     13 
"     ...    13 
"     ...    13 
"     ...    13 
"      ...     13 
"     ...    13 

12    15 
10      0 
10    45 
11      0 
11     30 
11     35 
12      0 
11     34 
12     26 
12    51 
13      0 
13      0 
13      0 
13      4 

14       0 
15    30 
18      0 
!  18     11 
17    30 
13    20 
17    54 
17    40 
14    20 
17     15 



.1     3 

16    30 

572 

I.  •* 

••••'   " 





a  —  152°  6  —  +  18°                         1 

3 

17    27 
!  17      0 

"17"  "ib" 

1,402 
1,400 

,  'l,545 

In  Leo                                          lo 

2 

i 

17     28 
18      0 
17    37 

'leT'sb" 

1   i 

628 

4 

•5 

207.  A.  J.  S.  XLIIIo,  78. 
208.        "              " 
209.   A.  J.  S.  XLIIIo,  413. 
210.   A.  J.  S.  XLIIIo,  78. 
211.  A.  J.  S.  XLIII2,  78;  Nov.  Meteors,  1866, 
U.  S.  N.  Obs'y,  8vo. 
212.   A.  J.  S.  XLIIIo,  78. 

214!  A.  J.  S.  XLIIIo,  78;  Nov.  Meteors,  1866, 
U.  S.  N.  Obs'y,  8vo. 
215. 
216.  Trans.  St.  Louis  Acad.  Sci.,  II,  577. 
217.   A.  J.  S.  XLIVo,  426. 
218.        " 
219. 

220.   A.  J.  S.  XLIVo,  426. 
221.        "             "     "    " 
222.        "             " 
223.        "              "           " 
224.  A.  J.  S.  XLVo,  78. 
225.        "            "     "    " 
226.   A.  J.S.  XLVo,  225. 
227.   A.  J.  S.  XLVg,  78. 
228.  Smithsonian  Archives  (not  yet  printed). 
229.   A.  J.  S.  XLVo,  225. 

230.   A.  J.  S.  XLVo,  78. 
231. 
'    232.  Proc.  Am.  Phil.  Soc.  X,  356. 
233.   A.  J.  S.  XLVo,  78. 
234.        "              "  "     " 

PROGRESS  OF   METEORIC   ASTRONOMY   IN   AMERICA. 
HVIeteor   Showers— Cont'd. 


333 


Ref.  number. 

Authority. 

Place  of  observation. 

Remarks. 

207 

B.  V.  Marsh  

Germantown,  Pa 

208 
209 
210 
211 

Prof.  A.  C.  Twining  
The  Denver  News  
W.  A.  Anthony  
James  Ferguson  

New  Haven,  Conn. 
Denver,  Col. 
Franklin,  N.  Y. 
U.  S.  Naval  Observatory. 

212 
213 

Prof.  A.  C.  Twining  
Maria  Mitchell  

New  Haven,  Conn. 
Vassar  College,  N.  Y. 

214 

James  Ferguson  

II.  8.  Naval  Observatory 

120  tracks  plotted  on  charts  from  Nov. 

215 

U  S  Naval  Observatory 

9  to  Nov  17   inclusive 

216 

R.  Hayes  

St.  Louis,  Mo  

Observations  made  in  the  evening. 

217 

F  W.  Russell 

Winchendon  Mass 

"  Moon  two  days  past  the  full  " 

218 

B.  V.  Marsh  

Philadelphia,  Pa. 

219 

220 

C.  H.  Darlington  
Lewis  Swift  

Philadelphia,  Pa. 
Marathon,  N.  Y. 

221 

F.  W  Russell        .     .. 

Winchendon  Mass 

222 

Lewis  Swift-  

Marathon,  N.  Y. 

223 

F.  W.  Russell 

Winchendon,  Mass. 

224 

Prof.  T.  C.  Wylie  

Bloomlngton,  Ind. 

225 
226 

Prof.  H.  A.  Newton  
Prof  N  R  Leonard 

New  Haven,  Conn. 
Iowa  City  Iowa          .. 

Cloudy  from  12h.  Om.  to  15h.  15m. 

227 

S.  J.  Gummere    

Haverford  College,  Pa. 

228 

Prof  F  H  Snow 

Lawrence  Kan 

229 

Prof  C  A  Young 

Hanover  N  H 

Dartmouth  College. 

230 

Prof.  T  H  Safford  

Chicago  111 

Number  of  observers  varied  from  8 

231 

Francis  Bradley  

Evanstown,  111. 

to  30. 

232 

James  McClure 

Philadelphia,  Pa   

Several  observers. 

233 
234 

San  Francisco  Times.. 
Prof.  H  A.  Newton 

San  Francisco,  Cal. 
New  Haven,  Conn   

One-third  of  the  sky  covered  with 

235 

G.  F.  Kingston  

Toronto,  Canada. 

clouds. 

236 
237 

Robert  B.  Taber  
Profs  Newcomb  and 

New  Bedford,  Mass. 
U.  S  N  Observatory      

147  tracks  mapped. 

238 
239 
240 
241 
242 

Eastman. 
Prof.  J.  C.  Watson  
Prof.  W.  Harkness  
Mrs.  J.  H.Trumbull... 
Prof.  G.  W.  Hough  
J.  N.  Flint          .      .  .. 

Ann  Arbor,  Mich. 
Richmond,  Va. 
Hartford,  Conn. 
Dudley  Observatory  
Canaseraga,  N.  Y. 

*In  Chihuahua,  Mexico,  the  meteors 
fell  so  fast  they  could  not  be  counted; 

243 
244 

Prof.  A.  C.  Twining  
J.  D.  Parker           

New  Haven,  Conn. 
Topeka,  Kan. 

often  20  or  30  visible  at  once. 

245 

Prof  E  Loomis 

New  Haven  Conn  

Observed  one  hour. 

240 
247 

C.  G.  Rockwood  
Robert  B  Taber 

Durham,  Conn. 
New  Bedford  Mass  

Actual  observing  time  4h.  35m. 

248 
249 

G.  T.  Kingston.... 
T  A.  Wylie 

Toronto,  Canada. 
Bloomington,  Ind. 

250 

W  S  Gilman  Jr 

Palisades   N  Y    

f  Several  bright  meteors  were  seen 

251 

B.  J  Gilman  '              . 

Williamstown,  Mass. 

during  the  Nov.  shower  in  1868. 

252 
253 
254 
255 
256 

Prof.  H.  A.  Newton  
S.  J.  Gummere  
Prof.  J.  R.  Eastman  ... 
C.  G.  Rockwood  
Lewis  Swift 

New  Haven,  Conn. 
Haverford  College,  Pa. 
U.  S.  N.  Observatory. 
Brunswick,  Me. 
Marathon,  N.  Y  

The  time  when  observations  ended 

257 

P.  E.  Chase 

Haverford  College,  Pa. 

not  given. 

258 

W.  H.  Pratt  

Davenport,  Iowa  

43  were  counted  before  13h.  Om. 

259 

C.  G.  Berner  

Vevay,  Ind. 

235.   A 

.  J.  S.  XLV2,  78. 

249. 

236. 

(4                            U                «* 

250. 

237.   A 

.  J.  S.  XLVs,  225;    Nov.  Meteors,  186», 

251. 

U.  S.  N.  Obs'y,  8vo. 

252. 

238.   A 

.  J.  S.  XLV2,  78. 

253. 

239.   A 

.  J.  S.  XLV2,  225;   Nov.  Meteors,  1867, 

254. 

240.   A 

U.  S.  N.  Obs'y,  8vo. 
.  J.  S.  XLV2,  78. 

255. 
256. 

241. 

it            U        n 

257. 

242. 

1C                           it                it 

243. 

«t            >t        It 

258. 

244. 

tt               II         It 

245. 

(1            11        It 

259. 

246.   A 

.  J.  S.  XLVII«,  287, 

247.   A 

.  J.  S.  XLVllo,  118. 

248. 

U                 it          t» 

A.  J.  S.  XLVII2,  118. 


Nov.  Meteors,  1868,  U.  S.  N.  Obs'y,  8vo. 
A.  J.  S.  XL VII2, 118. 

A.  J.  S.  XLVII2,  118 ;  Proc.  Am.  Phil.  Soc. 

X  539 
A.  J.'  S.  XLVII2, 118 ;  Dav.  Acad.  Nat.  Sei. 

1,14. 

A.  J.  S.  XLVII2, 118. 
*A.  J.  S.  XLV2,  78. 
fA.J.S.  XLVII2,399. 


334 


EASTMAN. 


I* 

o> 

^ 

g 

3 
C 

2 

260 
261 
262 
263 
264 
265 
266 
267 
268 
269 
270 
271 
272 
273 
274 
275 
276 
277 
278 
279 
280 
281 
282 
283 
284 
285 

286 
287 
288 
289 
290 
291 
292 

DATE. 

TIME  OF  SHOWER. 

Time  of  max. 
flight. 

Whole  num- 
ber counted. 

>> 

L 
f 

1 

ti 
"> 

I 
Radiant  point. 

0 

& 

Year 

Month. 

£ 

« 

13 

Begin- 
ning. 

End. 

1868 
1868 
1868 
1868 
1868 
1868 
1868 
1869 
1869 
1870 
1870 
1870 
1870 
1870 
1871 
1871 
1872 
1872 
1872 
1872 
1872 
1872 
1872 
•1875 
1876 
1876 

1877 
1885 
1885 
1885 
1885 
188  •> 
1885 

Nov 

h.     m. 

h.     m. 

h.     m. 
14    30 
16    55 

3,766 
4,278 
1,780 
455 
711 
250 
833 
830 
556 
31 
153 
82 
13 
11 
283 
98 
358 
62 
217 
80 
720 
143 
1,750 
112 
58 
12 

54 
44 
12 
13 
100 
213 
328 

900 
1,650 

5 

(i 

«i 

«< 

(i 

Aug.  '.'.'. 

Nov. 

13 
13 
13 
13 
13 
13 
13 
13 
12 
13 
13 
13 
13 
10 
11 

14    20 
15      0 
15      7 
15    30 
16      0 
16    30 
7      0 
13    18 
12    30 
11      6 
13     20 
13    30 
13    30 
11    40 

17    68 
17      0 
17    38 
18      0 
17     15 
17    30 
19      0 
15    43 
15    30 
15    45 
16    10 
15      0 
15      0 
13    18 

4 

1     3 

1 

1 



1 

2 



4 

2 





In  Leo                      :5 

"                                            :>, 





'.  i 

0 

Aug.  ... 
Nov.  '.'.! 

AUK.  '.". 

Get  
Nov.  ... 

«• 

1C 

9 
9 
24 

25 
27 
27 
27 
5 
24 
13 

13 

27 

27 
27 
27 
27 
27 

10    30 
14    45 
7    30 
10    25 
6      5 
6    10 
6    38 
13    30 
11    30 
12      0 

13    55 
6      0 
9      0 
10    15 
7    15 
6    30 
7      0 

15    30 
15    55 
12    30 
14      0 
10      0 
11     45 
8    48 
15    30 
15    30 
13      0 

15    45 
6    24 



4 

1 



2°or3°N  of  y  Andromeda' 

6    30 
............ 

300 

"i'soo* 

//.  Andromeda                               1 

a  =>  15°,  S  =  +  30°  1 
a  =  25°,  &  —  +  43°                            4 

In  Perseus                                     1 

Bet.  Orion  and  the  Pleiades..      1 
1 





In  Leo 

1 



y  Andromedce                           .    .'i 

10    30 
7    45 
7    50 
9      0 



2°N.  W.  ofyAndroiiifd.-i-  1 
;{ 

i 

260.  A.  J.  S.  XLVII2,  118. 

261.  Nov.  Meteors,  1868,  U.  S.  N.  Observatory, 

8  vo. 

262.  A.  J.  S.  XLVII2, 118. 

263.  "  "  " 

264.  "  " 

265.  "  "          " 

266.  "  "          " 

267.  A.  J.  S.  XLIX2,  244. 


268.  A.  J.  S.  XLIX2,  244. 

269.  A.  J.  S.  I3,  30.  " 

270.  "         "     " 

271.  "         "     " 

272.  "        "     " 

273.  "        "     " 

274.  A.  J.S.  1 13,  227. 

275.  A.  J.S.  II3,  470. 

276.  A.  J.S.  IV3,  244. 


PROGRESS   OF   METEORIC   ASTRONOMY   IN   AMERICA. 
Meteor    Showers— Cont'd., 


335 


Ref.  number.  I 

Authority. 

Place  of  observation. 

Remarks. 

260 

Maria  Mitchell 

Vas^ar  College  N  Y 

261 

Prof  J   R  Eastman 

U.S.  N.  Observatory  

90  tracks  plotted 

262 

B  J  Oilman 

Williamstown  Mass 

263 

C  W  Tuttle        

Boston,  Mass  

No  observations  between  16h  4m.  and 

264 

Robert  B  Taber 

New  Bedford  Mass. 

16h  33m 

265 

J.  E.  Hendricks  

Des  Moines,  Iowa. 

266 

B  F  Mudge 

Manhattan,  Kan. 

267 

Frederickton,  N.  B  

Reported  by  Prof.  H.  A.  Newton. 

268 
269 
270 
271 

979 

George  Davidson  
Prof.  H.  A.  Newton  
Prof.  H.  A.  Newton  
C.  G.  Rockwood  
B.  V    Marsh        . 

Santa  Barbara,  Cal. 
New  Haven,  Conn. 
New  Haven,  Conn. 
Brunswick,  Me  
Burlington,  N.  J. 

6  tracks  plotted. 

273 

274 

275 

J.  G.  Gummere  
Prof.  H.  A.  Newton  
Prof  H  A    Newton 

Burlington,  N.  J. 
Sherburne,  N.  Y. 
New  Haven,  Conn     

Only  a  few  belonged  to  the  November 

276 
277 
278 
279 
280 
281 

Prof.  C.  A.  Lyman  
R.  W.  McFarland  
Prof.  H.  A.  Newton  
Prof.  H.  A.  Newton  
Prof.  J.  R.  Eastman  ... 
B.  V.  Marsh        

New  Haven,  Conn. 
Oxford,  Ohio. 
New  Haven,  Conn. 
New  Haven,  Conn. 
U.  S.  N.  Observatory. 
Philadelphia,  Pa. 

system. 

282 
283 

Prof.  H.  A.  Newton  
Prof.  J.  R.  Eastman 

New  Haven,  Conn. 
U.  S.  N.  Observatory  

Most  of  the  meteors  had  short  trains. 

284 
•W 

Prof.  J.  R.  Eastman  ... 
Prof.  H.  A.  Newton  .   . 

U.  S.  N.  Observatory  
New  Haven,  Conn  

A  few  left  long  trains. 
Night  mostly  cloudy;  3  conformable 

286 

Prof  D  Kirkwood 

Bloomington   Ind 

to  radiant. 
Night  mostly  cloudy. 

287 
288 

Robert  Brown  

H  A  Newton 

New  Haven,  Conn. 
New  Haven  Conn         

Hourly  number  estimated  for  3  ob- 

289 
290 

H.  A.  Newton  ... 

New  Haven,  Conn. 
Princeton,  N.  J 

servers,  100. 

291 

A.  Hall    

Georgetown,  D.  C. 

?W 

D.  Horigan  

Georgetown,  D.  C. 

277.  A.  J.  S.  IV3,  244. 

278.  A.  J.  S.  V3,  53. 

279.  "          "     " 

280.  "          "     " 

281.  "  "     " 

282.  "  "     " 

283.  Astron'l  and  Meteor'l  Observ'ns,  1875. 

284.  Astrou'l  and  Meteor'l  Ob.serv'ns,  187C. 


285.  A.  J.  S.  XII3,  473. 

286.  A.  J.  S.  XV3,  76. 

287.  A.  J.  S.  XXXIs,  78. 

288.  " 

289.  " 

290.  "  "  " 

291.  "  " 

292.  "  "  " 


336 


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343 


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PROGRESS   OP   METEORIC   ASTRONOMY  IN   AMERICA.  345 


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D.  Horigan. 
D.  Horigan. 
D.  Horigan. 
Prof.  J.  R.  Eastman. 

Wash'n  Ast.  &  Met.  Obs'ns,  1870. 

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Remarks. 

j 

C 

< 
«c 
j 

PI 

.  Across  the  "Sickle  "  
.  From  a  point  on  the  meridian  10°  S  , 

Smith  nf  „  f'onia  Mainria 

.  Northerly  from  near  the  eastern  horizon  
.  Northerly  from  near  the  eastern  horizon  
.  Northerly  from  near  the  eastern  horizon  
.  Across  the  "Dinner"  ... 

of  a  Bootis  
lation  of  the  Scorpion  

>laris  
arallel  to  the  above  course.. 

er  small  meteors,  all  mov- 

• 

.  From  10°  south  of  the  zenith  

.  From  £  Ursee  Minoris  to  5°  south 
.  From  alt.  40°  through  the  conste 

.  From  /3  Cassiopese  to  10°  below  P< 
.  Exactly  across  Polaris  in  a  line  p 

.  Between  9h.  and  lOh.  saw  ten  oth 
ing  westward. 

i 

c 
i 

ii 

&.~*~ 
5| 

li 

t  C 

s  a 

, 

91.  Wash'n  Ast.  A  Met.  Obs'ns,  1870.  96.  Wash'n  A«t.  &  Met.  Obs'ns,  1870.  101 
92.  97.  ••  "  "  102 
93.  98.  "  "  "  103. 
94.  99.  "  "  "  104. 
95.  100.  " 

Direction  of  motion. 

: 

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PL 

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to 

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Towards  the  W  
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N.W.  from  a  Cygni  . 
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> 

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1 

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PROGRESS  OF   METEORIC   ASTRONOMY   IN   AMERICA.  347 


Observer. 

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with  a  Iou 

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i 
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l 

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1 
1 

i 

Very  brilliant  
Burst  into  three  fragments 

Very  brilliant  

Very  brilliant  

Seen  at  several  other  citie. 
Motion  seemed  to  be  by  in 

Direction  of  motion. 

Southwest  

1 

55* 

id 

'  3 

<£ 

From  West  to  East  
Fell  vertically  from  a  Cassiopese 

Towards  v  Ursa  Majoris  

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43-Bull.  Phil.  Soc.,  Wash.,  Vol.  11. 


348 


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PROGRESS   OF   METEORIC   ASTRONOMY    IN   AMERICA. 


351 


Observer. 

1 

W2a 

Q(XC 

CS                              ^3 

1  f  1  1 

L76.  Wash'n  Ast.  &  Met.  Obs'ns,  1876. 
177. 
78. 
79.  "  " 
80. 

j        Tsg-a-c-r!.        STSD:^     ncooaaaoaa 

!           •d?'O-a'O02            X'O^Sfed       eSsSoSJnoSS^SSoS 

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..P1"-   •  •   •          .   -^o   .     o  o  o^  o  o  o  o  o  o 

PH  PH  P-i  Pi  3n  Q          u£n'£td<Q      W  WM<33  W  W  WHS 

)         QQQQQtXi         ciJQa.QQH     QQQOQQQQQQ 

Kemarks. 

• 

Exploded  and  illuminated  the  small  cloud  behind  which  it 
passed. 

All  disappeared  at  an  altitude  of  5°  1 

Within  6°  or  8°  of  the  horizon  it  passed  behind  a  bank  of 
clouds. 

Seen  in  Missouri,  Kansas,  Iowa,  Nebraska,  and  Ohio  

M 

o 

c 

m 

S 

1 

6 

0 

S 
3 

CO 

Exploded  over  Lake  Michigan  at  an  altitude  of  34  miles  

h'n  Ast.  &  Met.  Obs'ns,  1876. 

iC  K  .1 
1C  ,«  « 

" 

ii  i; 

Direction  of  motion. 

> 

| 

| 
i 

vertically. 

> 

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i 

a 

/- 

•>> 

- 

Q 

"£ 
a 

_/ 

^ 

c. 

t 

a 

> 

| 
I 

Moved  vertically  through  e 
Cygui  and  nearly  through  j8 
Cygni. 

• 

o^i 

c'c 

ll 

From  N.  78°  W.  over  N.  E.  cor- 
ner of  Indiana. 

j 

\ 

T 
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£ 

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c  a 

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sfl 

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cos  w 

West  across  Polaris  ... 

N  K  frnm  fi  Pptraai 

S.  W.  from  Polaris  
E.  S.  E.  from  Saturn.... 

1 
jf  £!J2?i£ 

L65.  Wash'n  Ast.  &  Met.  Obs'ns,  1875. 
00.  Trans.  St.  Louis  Acad.  8ci.  Ill,  349. 
67.  Astron'l  and  Meteor'l  Observations,  1876. 
168.  A.  J.  S.  XI8,  458. 
09.  Wash'n  Ast.  &  Met.  Obs'ns,  187C. 
170.  A.  J.  S.  XIV3,75. 

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352 


EASTMAN. 


PROGRESS  OF   METEORIC   ASTRONOMY   IN   AMERICA. 


353 


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PROGRESS  OF   METEORIC    ASTRONOMY   IN    AMERICA.  355 


Observer. 

_. 

H.  E.  Stevens. 
J.  J.  Skinner. 

232.  Science  Observer,  1,  36.  1  234.  Science  Observer,  II,  30. 
233.  Proc.  Am.  Phil.  Soc.  XVIII,  241.  235. 

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J 

'o 

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'o>     t 

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so  ; 

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.  Supposed  to  have  been  seen  in  Oil  City  and  Titusville,  Pa... 

i 

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